Globular cluster

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Thousands of white-ish dots scattered on a black background, strongly concentrated towards the centre
The Messier 80 globular cluster in the constellation Scorpius is located about 30,000 light-years from the Sun and contains hundreds of thousands of stars.[1]

A globular cluster is a spherical collection of stars. Globular clusters are very tightly bound by gravity, which gives them their spherical shapes and high stellar densities toward their centers. The name of this category of star cluster is derived from the Latin, globulus—a small sphere. Occasionally, a globular cluster is known simply as a globular.

Globular clusters in spiral galaxies are mostly found in the galactic halo. Globular clusters tend to be older, more massive, denser, and contain fewer heavy elements than open clusters, which are generally found in the disks of spiral galaxies. Globular clusters are fairly common; there are over 150[2][3] known in the Milky Way, with possibly many more still to be found.[4] The Andromeda Galaxy, comparable in size to the Milky Way, may have as many as 500.[5] Some giant elliptical galaxies (particularly those at the centers of galaxy clusters), such as M87, have as many as 13,000 globular clusters.[6]

Every galaxy of sufficient mass in the Local Group has an associated group of globular clusters, and almost every large galaxy surveyed has been found to possess a system of globular clusters.[7] Some globular clusters likely originally formed in dwarf galaxies and have since been removed from their birth galaxies by tidal forces and joined the Milky Way.

Although it appears that globular clusters contain some of the first stars to be produced in the galaxy, their origins and their role in galactic evolution are still unclear. However, it does appear clear that globular clusters are significantly different from dwarf elliptical galaxies and were formed as part of the star formation of the parent galaxy, rather than as a separate galaxy.[8]

Observation history[edit]

Early globular cluster discoveries
Cluster name Discovered by Year
M 22[9] Abraham Ihle 1665
ω Cen[10][a] Edmond Halley 1677
M 5[11][12] Gottfried Kirch 1702
M 13[13] Edmond Halley 1714
M 71[14] Philippe Loys de Chéseaux 1745
M 4[14] Philippe Loys de Chéseaux 1746
M 15[15] Jean-Dominique Maraldi 1746
M 2[15] Jean-Dominique Maraldi 1746

The first known globular cluster, now called M 22, was discovered in 1665 by Abraham Ihle, a German amateur astronomer.[9][16] Given the small aperture of early telescopes, individual stars within a globular cluster were not resolved until Charles Messier observed M 4 in 1764.[17][18] Subsequently, Abbé Lacaille would list NGC 104, NGC 4833, M 55, M 69, and NGC 6397 in his 1751–1752 catalogue.[b]

When William Herschel began his comprehensive survey of the sky using large telescopes in 1782 there were 34 known globular clusters. Herschel discovered another 36 himself and was the first to resolve virtually all of them into stars. He coined the term "globular cluster" in his Catalogue of a Second Thousand New Nebulae and Clusters of Stars published in 1789.[19][20]

The number of globular clusters discovered continued to increase, reaching 83 in 1915, 93 in 1930, 97 by 1947,[20] and 157 in 2010.[2] Additional, undiscovered globular clusters are believed to be hidden behind the gas and dust of the Milky Way.[21]

Beginning in 1914, Harlow Shapley began a series of studies of globular clusters, published in about 40 scientific papers. He examined the RR Lyrae variables in the clusters (which he assumed were Cepheid variables) and used their period–luminosity relationship for distance estimates. Later, it was found that RR Lyrae variables are fainter than Cepheid variables, which caused Shapley to overestimate the distances of the clusters.[22]

Thousands of white-ish dots scattered on a black background, strongly concentrated towards the centre
NGC 7006 is a highly concentrated, Class I globular cluster.

Of the globular clusters within the Milky Way, the majority are found in a halo around the galactic core, and the large majority are located in the celestial sky centered on the core. In 1918, this strongly asymmetrical distribution was used by Shapley to make a determination of the overall dimensions of the galaxy. By assuming a roughly spherical distribution of globular clusters around the galaxy’s center, he used the positions of the clusters to estimate the position of the Sun relative to the galactic center.[23] While his distance estimate was in significant error (although within the same order of magnitude as the currently accepted value), it did demonstrate that the dimensions of the galaxy were much greater than had been previously thought.[c]

Shapley's measurements indicated that the Sun is relatively far from the center of the galaxy, also contrary to what had previously been inferred from the apparently nearly even distribution of ordinary stars. In reality, most ordinary stars lie within the galaxy's disk and those stars that lie in the direction of the galactic centre and beyond are thus obscured by gas and dust, whereas globular clusters lie outside the disk and can be seen at much further distances.[22]

Classification[edit]

Shapley was subsequently assisted in his studies of clusters by Henrietta Swope and Helen Battles Sawyer (later Hogg). In 1927–1929, Shapley and Sawyer categorized clusters according to the degree of concentration each system has toward its core. The most concentrated clusters were identified as Class I, with successively diminishing concentrations ranging to Class XII.[d] This became known as the Shapley–Sawyer Concentration Class.[24] In 2015, a new type of globular cluster was proposed on the basis of observational data: dark globular clusters.[25]

Formation[edit]

Thousands of white-ish dots scattered on a black background, strongly concentrated towards the centre
NGC 2808 contains three distinct generations of stars.[26] NASA image

The formation of globular clusters is and still remains poorly understood. Traditionally, globular clusters have been described as a simple stellar population, in which all of the stars formed from the same giant molecular cloud and thus have roughly the same age and metallicity. However, modern observations show that nearly all globular clusters contain multiple populations.[27] An example of this is the globular clusters in the Large Magellanic Cloud (LMC) that exhibit a bimodal population. During their youth, these LMC clusters may have encountered giant molecular clouds that triggered a second round of star formation.[28] This star-forming period is relatively brief, compared with the age of many globular clusters.[29] It has been proposed that the reason for this multiplicity in stellar populations could have a dynamical origin. In the Antennae galaxy, for example, the Hubble Space Telescope has observed clusters of clusters, regions in the galaxy that span hundreds of parsecs, where many of the clusters will eventually collide and merge. Many of them present a significant range in ages, hence possibly metallicities, and their merger could plausibly lead to clusters with a bimodal or even multiple distribution of populations.[30]

A small fuzzy white ball in the centre of a speckled black backdrop
Globular star cluster Messier 54[31]

Observations of globular clusters show that these stellar formations arise primarily in regions of efficient star formation, and where the interstellar medium is at a higher density than in normal star-forming regions. Globular cluster formation is prevalent in starburst regions and in interacting galaxies.[32] Research indicates a correlation between the mass of a central supermassive black holes (SMBH) and the extent of the globular cluster systems of elliptical and lenticular galaxies. The mass of the SMBH in such a galaxy is often close to the combined mass of the galaxy's globular clusters.[33]

No known globular clusters display active star formation, which is consistent with the view that globular clusters are typically the oldest objects in the Galaxy and were among the first collections of stars to form. Very large regions of star formation known as super star clusters, such as Westerlund 1 in the Milky Way, may be the precursors of globular clusters.[34]

Composition[edit]

A loose scattering of small dull white dots on a black background with a few brighter coloured stars
Djorgovski 1's stars contain hydrogen and helium, but not much else. In astronomical terms, they are described as "metal-poor".[35]

Globular clusters are generally composed of hundreds of thousands of low-metal, old stars. The type of stars found in a globular cluster are similar to those in the bulge of a spiral galaxy but confined to a volume of only a few million cubic parsecs. They are free of gas and dust and it is presumed that all of the gas and dust was long ago either turned into stars or blown out of the cluster during the initial burst of star formation.

Globular clusters can contain a high density of stars; on average about 0.4 stars per cubic parsec, increasing to 100 or 1000 stars per cubic parsec in the core of the cluster.[36] The typical distance between stars in a globular cluster is about 1 light year,[37] but at its core, the separation is comparable to the size of the Solar System (100 to 1000 times closer than stars near the Solar System).[38]

Globular clusters are not thought to be favorable locations for the survival of planetary systems. Planetary orbits are dynamically unstable within the cores of dense clusters because of the perturbations of passing stars. A planet orbiting at 1 astronomical unit around a star that is within the core of a dense cluster such as 47 Tucanae would only survive on the order of 108 years.[39] There is a planetary system orbiting a pulsar (PSR B1620−26) that belongs to the globular cluster M 4, but these planets likely formed after the event that created the pulsar.[40]

Some globular clusters, like Omega Centauri in the Milky Way and G 1 in M 31, are extraordinarily massive, with several million solar masses (M) and multiple stellar populations. Both can be regarded as evidence that supermassive globular clusters are in fact the cores of dwarf galaxies that are consumed by the larger galaxies.[41] About a quarter of the globular cluster population in the Milky Way may have been accreted along with their host dwarf galaxy.[42] More than 60% of the globular clusters in the outer halo (more than 25 kiloparsecs (82,000 ly) from the center) of the Andromeda Galaxy were likely accreted in a similar fashion.[43]

Heavy element content[edit]

Thousands of white-ish dots scattered on a black background, strongly concentrated towards the centre
Messier 53 contains an unusually large number of a type of star called "blue stragglers".[44][45]

Globular clusters normally consist of Population II stars, which have a low proportion of elements other than hydrogen and helium when compared with Population I stars such as the Sun. Astronomers refer to these heavier elements as metals and to the proportions of these elements as the metallicity. These elements are produced by stellar nucleosynthesis and then are recycled into the interstellar medium, where they enter the next generation of stars. Hence the proportion of metals can be an indication of the age of a star, with older stars typically having a lower metallicity.[46]

The Dutch astronomer Pieter Oosterhoff noticed that there appear to be two populations of globular clusters, which became known as Oosterhoff groups. The second group has a slightly longer period of RR Lyrae variable stars.[47] Both groups have weak spectral lines of metallic elements. But the lines in the stars of Oosterhoff type I (Oo I) cluster are not quite as weak as those in type II (Oo II).[47] Hence type I are referred to as "metal-rich" (for example, Terzan 7[48]), while type II are "metal-poor" (for example, ESO 280-SC06[49]).

These two populations have been observed in many galaxies, especially massive elliptical galaxies. Both groups are nearly as old as the universe itself and are of similar ages, but differ in their metal abundances. Many scenarios have been suggested to explain these subpopulations, including violent gas-rich galaxy mergers, the accretion of dwarf galaxies, and multiple phases of star formation in a single galaxy. In the Milky Way, the metal-poor clusters are associated with the halo and the metal-rich clusters with the bulge.[50]

In the Milky Way it has been discovered that the large majority of the low metallicity clusters are aligned along a plane in the outer part of the galaxy's halo. This result argues in favor of the view that type II clusters in the galaxy were captured from a satellite galaxy, rather than being the oldest members of the Milky Way's globular cluster system as had been previously thought. The difference between the two cluster types would then be explained by a time delay between when the two galaxies formed their cluster systems.[51]

Exotic components[edit]

Globular clusters have a very high star density, and therefore close interactions and near-collisions of stars occur relatively often. Due to these chance encounters, some exotic classes of stars, such as blue stragglers, millisecond pulsars, and low-mass X-ray binaries, are much more common in globular clusters. A blue straggler is thought to form from the merger of two stars, possibly as a result of an encounter with a binary system.[52] The resulting star has a higher temperature than comparable stars in the cluster with the same luminosity, and thus differs from the main sequence stars formed at the beginning of the cluster.[53]

Hundreds of white-ish dots scattered on a black background, concentrated towards the centre
Globular cluster M15 may have an intermediate-mass black hole at its core. NASA image.

Astronomers have searched for black holes within globular clusters since the 1970s. The resolution requirements for this task are exacting, and it is only with the Hubble Space Telescope that the first claimed discoveries were made. In independent programs, a 4,000 M intermediate-mass black hole was suggested to exist based on HST observations in the globular cluster M 15 and a 20,000 M black hole in the Mayall II cluster in the Andromeda Galaxy.[54] Both x-ray and radio emissions from Mayall II appear to be consistent with an intermediate-mass black hole.[55] However, these claimed detections are controversial.[56] The heaviest objects in globular clusters are expected to migrate to the cluster center due to mass segregation. As pointed out in two papers by Holger Baumgardt and collaborators, the mass-to-light ratio should rise sharply towards the center of the cluster, even without a black hole, in both M 15[57] and Mayall II.[58]

Confirmed intermediate-mass black holes in globular clusters would be significant for theories of galactic development and as possible sources for the supermassive black holes at their centres. The mass of these intermediate mass black holes is proportional to the mass of the clusters, following a pattern previously discovered between supermassive black holes and their surrounding galaxies.[56][59]

Color-magnitude diagram[edit]

Thousands of white-ish dots scattered on a black background, concentrated towards the left side of the frame
Messier 5 is a globular cluster consisting of hundreds of thousands of stars bound together by their collective gravity.[60]

The Hertzsprung-Russell diagram (HR-diagram) is a graph of a large sample of stars that plots their visual absolute magnitude against their color index. The color index, B−V, is the difference between the magnitude of the star in blue light, or B, and the magnitude in visual light (green-yellow), or V. Large positive values indicate a red star with a cool surface temperature, while negative values imply a blue star with a hotter surface.

When the stars near the Sun are plotted on an HR diagram, it displays a distribution of stars of various masses, ages, and compositions. Many of the stars lie relatively close to a sloping curve with increasing absolute magnitude as the stars are hotter, known as main-sequence stars. The diagram also typically includes stars that are in later stages of their evolution and have wandered away from this main-sequence curve.

As all the stars of a globular cluster are at approximately the same distance from the Earth, their absolute magnitudes differ from their visual magnitude by about the same amount. The main-sequence stars in the globular cluster will fall along a line that is believed to be comparable to similar stars in the solar neighborhood. The accuracy of this assumption is confirmed by comparable results obtained by comparing the magnitudes of nearby short-period variables, such as RR Lyrae stars and cepheid variables, with those in the cluster.[61]

By matching up these curves on the HR diagram the absolute magnitude of main-sequence stars in the cluster can be determined. This in turn provides a distance estimate to the cluster, based on the visual magnitude of the stars. The difference between the relative and absolute magnitude, the distance modulus, yields this estimate of the distance.[62]

When the stars of a particular globular cluster are plotted on an HR diagram, in many cases nearly all of the stars fall upon a relatively well-defined curve. This differs from the HR diagram of stars near the Sun, which lumps together stars of differing ages and origins. The shape of the curve for a globular cluster is characteristic of a grouping of stars that were formed at approximately the same time and from the same materials, differing only in their initial mass. As the position of each star in the HR diagram varies with age, the shape of the curve for a globular cluster can be used to measure the overall age of the star population.[63]

However, the above-mentioned historic process of determining the age and distance to globular clusters is not as robust as first thought, since the morphology and luminosity of globular cluster stars in color-magnitude diagrams are influenced by numerous parameters, many of which are still being actively researched. Certain clusters even display populations that are absent from other globular clusters (e.g., blue hook stars), or feature multiple populations. The historical paradigm that all globular clusters consist of stars born at exactly the same time, or sharing exactly the same chemical abundance, has likewise been overturned (e.g., NGC 2808).[64] Further, the morphology of the cluster stars in a color-magnitude diagram, and that includes the brightnesses of distance indicators such as RR Lyrae variable members, can be influenced by observational biases. One such effect is called blending, and it arises because the cores of globular clusters are so dense that in low-resolution observations multiple (unresolved) stars may appear as a single target. Thus the brightness measured for that seemingly single star (e.g., an RR Lyrae variable) is erroneously too bright, given those unresolved stars contributed to the brightness determined.[65] Consequently the computed distance is wrong, so the blending effect can introduce a systematic uncertainty into the cosmic distance ladder and may bias the estimated age of the Universe and the Hubble constant.[66]

A scattering of dots on a black background, most yellow and aligned in a roughly vertical band down the centre, with some white dots extending in two arms to the left and a few red dots scattered on the right of the image
Color-magnitude diagram for the globular cluster M3. Note the characteristic "knee" in the curve at magnitude 19 where stars begin entering the giant stage of their evolutionary path.

The most massive main-sequence stars will have the highest absolute magnitude, and these will be the first to evolve into the giant star stage. As the cluster ages, stars of successively lower masses will also enter the giant star stage. Thus the age of a single population cluster can be measured by looking for the stars that are just beginning to enter the giant star stage. This forms a "knee" in the HR diagram, bending to the upper right from the main-sequence line. The absolute magnitude at this bend is directly a function of the age of globular cluster, so an age scale can be plotted on an axis parallel to the magnitude.

In addition, globular clusters can be dated by looking at the temperatures of the coolest white dwarfs. Typical results for globular clusters are that they may be as old as 12.7 billion years.[67] This is in contrast to open clusters which are rarely older than about 500 million years.[68]

The ages of globular clusters place a bound on the age limit of the entire universe. This lower limit has been a significant constraint in cosmology. Historically, astronomers were faced with age estimates of globular clusters that appeared older than cosmological models would allow.[69] However, better measurements of cosmological parameters through deep sky surveys and satellites such as the Hubble Space Telescope appear to have resolved this issue.[70][71]

Evolutionary studies of globular clusters can be used to determine changes due to the starting composition of the gas and dust that formed the cluster. That is, the evolutionary tracks change with changes in the abundance of heavy elements. The data obtained from studies of globular clusters are then used to study the evolution of the Milky Way as a whole.[38]

In globular clusters a few stars known as blue stragglers are observed, apparently continuing the main sequence in the direction of brighter, bluer stars. The origins of these stars is still unclear, but most models suggest that these stars are the result of mass transfer in multiple star systems.[52]

Morphology[edit]

Ellipticity of globular clusters
Galaxy Ellipticity[72]
Milky Way 0.07±0.04
LMC 0.16±0.05
SMC 0.19±0.06
M31 0.09±0.04

In contrast to open clusters, most globular clusters remain gravitationally bound for time periods comparable to the life spans of the majority of their stars. However, strong tidal interactions with other large masses result in the dispersal of the stars, leaving behind "tidal tails" of stars removed from the cluster.[73][74]

After they are formed, the stars in the globular cluster begin to interact gravitationally with each other. As a result, the velocity vectors of the stars are steadily modified, and the stars lose any history of their original velocity. The characteristic interval for this to occur is the relaxation time. This is related to the characteristic length of time a star needs to cross the cluster as well as the number of stellar masses in the system.[75] The value of the relaxation time varies by cluster, but a typical value is on the order of 109 years.[76]

Although globular clusters generally appear spherical in form, ellipticities can occur due to tidal interactions. Clusters within the Milky Way and the Andromeda Galaxy are typically oblate spheroids in shape, while those in the Large Magellanic Cloud are more elliptical.[77]

Radii[edit]

Hundreds of white-ish dots scattered on a black background, concentrated towards the centre, with a number of brighter red and blue dots scattered across the frame
NGC 411 is classified as an open cluster.[78]

Astronomers characterize the morphology of a globular cluster by means of standard radii. These are the core radius (rc), the half-light radius (rh), and the tidal (or Jacobi) radius (rt). The overall luminosity of the cluster steadily decreases with distance from the core, and the core radius is the distance at which the apparent surface luminosity has dropped by half.[79] A comparable quantity is the half-light radius, or the distance from the core within which half the total luminosity from the cluster is received. This is typically larger than the core radius.

The half-light radius includes stars in the outer part of the cluster that happen to lie along the line of sight, so theorists will also use the half-mass radius (rm)—the radius from the core that contains half the total mass of the cluster. When the half-mass radius of a cluster is small relative to the overall size, it has a dense core. An example of this is Messier 3 (M3), which has an overall visible dimension of about 18 arc minutes, but a half-mass radius of only 1.12 arc minutes.[80]

Almost all globular clusters have a half-light radius of less than 10 pc, although there are well-established globular clusters with very large radii (i.e. NGC 2419 (Rh = 18 pc) and Palomar 14 (Rh = 25 pc)).[81]

Finally the tidal radius, or Hill sphere, is the distance from the center of the globular cluster at which the external gravitation of the galaxy has more influence over the stars in the cluster than does the cluster itself. This is the distance at which the individual stars belonging to a cluster can be separated away by the galaxy. The tidal radius of M3 is about 40 arc minutes,[82] or about 113 pc[83] at the distance of 10.4 kpc.

Mass segregation, luminosity and core collapse[edit]

In measuring the luminosity curve of a given globular cluster as a function of distance from the core, most clusters in the Milky Way increase steadily in luminosity as this distance decreases, up to a certain distance from the core, then the luminosity levels off. Typically this distance is about 1–2 parsecs from the core. About 20% of the globular clusters have undergone a process termed "core collapse". In this type of cluster, the luminosity continues to increase steadily all the way to the core region.[84][85] Examples of core-collapsed globular clusters include M15 and M30.

Thousands of white-ish dots scattered on a black background, strongly concentrated towards the centre
47 Tucanae – the second most luminous globular cluster in the Milky Way, after Omega Centauri

Core-collapse is thought to occur when the more massive stars in a globular cluster encounter their less massive companions. Over time, dynamic processes cause individual stars to migrate from the center of the cluster to the outside. This results in a net loss of kinetic energy from the core region, leading the remaining stars grouped in the core region to occupy a more compact volume. When this gravothermal instability occurs, the central region of the cluster becomes densely crowded with stars and the surface brightness of the cluster forms a power-law cusp.[86] A core collapse is not the only mechanism that can cause such a luminosity distribution; a massive black hole at the core can also result in a luminosity cusp.[87] Over a lengthy period of time this leads to a concentration of massive stars near the core, a phenomenon called mass segregation.

The dynamical heating effect of binary star systems works to prevent an initial core collapse of the cluster. When a star passes near a binary system, the orbit of the latter pair tends to contract, releasing energy. Only after the primordial supply of binaries is exhausted due to interactions can a deeper core collapse proceed.[88][89] In contrast, the effect of tidal shocks as a globular cluster repeatedly passes through the plane of a spiral galaxy tends to significantly accelerate core collapse.[90]

The different stages of core-collapse may be divided into three phases. During a globular cluster's adolescence, the process of core-collapse begins with stars near the core. The interactions between binary star systems prevents further collapse as the cluster approaches middle age. Finally, the central binaries are either disrupted or ejected, resulting in a tighter concentration at the core.

The interaction of stars in the collapsed core region causes tight binary systems to form. As other stars interact with these tight binaries, they increase the energy at the core, which causes the cluster to re-expand. As the mean time for a core collapse is typically less than the age of the galaxy, many of a galaxy's globular clusters may have passed through a core collapse stage, then re-expanded.[91]

Hundreds of white-ish dots scattered on a black background, concentrated towards the centre
Globular cluster NGC 1854 is located in the Large Magellanic Cloud.[92]

The Hubble Space Telescope has been used to provide convincing observational evidence of this stellar mass-sorting process in globular clusters. Heavier stars slow down and crowd at the cluster's core, while lighter stars pick up speed and tend to spend more time at the cluster's periphery. The globular star cluster 47 Tucanae, which is made up of about 1 million stars, is one of the densest globular clusters in the Southern Hemisphere. This cluster was subjected to an intensive photographic survey, which allowed astronomers to track the motion of its stars. Precise velocities were obtained for nearly 15,000 stars in this cluster.[93]

The overall luminosities of the globular clusters within the Milky Way and the Andromeda Galaxy can be modeled by means of a gaussian curve. This gaussian can be represented by means of an average magnitude Mv and a variance σ2. This distribution of globular cluster luminosities is called the Globular Cluster Luminosity Function (GCLF). For the Milky Way, Mv = −7.20 ± 0.13, σ = 1.1 ± 0.1 magnitudes. The GCLF has been used as a "standard candle" for measuring the distance to other galaxies, under the assumption that the globular clusters in remote galaxies follow the same principles as they do in the Milky Way.[94]

N-body simulations[edit]

Computing the interactions between the stars within a globular cluster requires solving what is termed the N-body problem. That is, each of the stars within the cluster continually interacts with the other N−1 stars, where N is the total number of stars in the cluster. The naive CPU computational "cost" for a dynamic simulation increases in proportion to N 2 (each of N objects must interact pairwise with each of the other N objects), so the potential computing requirements to accurately simulate such a cluster can be enormous.[95][96] An efficient method of mathematically simulating the N-body dynamics of a globular cluster is done by subdividing into small volumes and velocity ranges, and using probabilities to describe the locations of the stars. The motions are then described by means of a formula called the Fokker–Planck equation. This can be solved by a simplified form of the equation, or by running Monte Carlo simulations and using random values. The simulation becomes more difficult when the effects of binaries and the interaction with external gravitation forces (such as from the Milky Way galaxy) must also be included.[97]

The results of N-body simulations have shown that the stars can follow unusual paths through the cluster, often forming loops and often falling more directly toward the core than would a single star orbiting a central mass. In addition, due to interactions with other stars that result in an increase in velocity, some of the stars gain sufficient energy to escape the cluster. Over long periods of time this will result in a dissipation of the cluster, a process termed evaporation.[98] The typical time scale for the evaporation of a globular cluster is 1010 years.[75] In 2010 it became possible to directly compute, star by star, N-body simulations of a low-density globular cluster over the course of its lifetime.[99]

Binary stars form a significant portion of the total population of stellar systems, with up to half of all field stars and open cluster stars occurring in binary systems.[100][101] The present-day binary fraction in globular clusters is difficult to measure, and any information about their initial binary fraction is lost by subsequent dynamical evolution.[102] Numerical simulations of globular clusters have demonstrated that binaries can hinder and even reverse the process of core collapse in globular clusters. When a star in a cluster has a gravitational encounter with a binary system, a possible result is that the binary becomes more tightly bound and kinetic energy is added to the solitary star. When the massive stars in the cluster are sped up by this process, it reduces the contraction at the core and limits core collapse.[53][103]

The ultimate fate of a globular cluster must be either to accrete stars at its core, causing its steady contraction,[104] or gradual shedding of stars from its outer layers.[105]

Intermediate forms[edit]

Thousands of white-ish dots scattered on a black background, strongly concentrated towards the centre
Messier 10 lies about 15,000 light-years from Earth, in the constellation of Ophiuchus.[106]

The distinction between cluster types is not always clear-cut, and objects have been found that blur the lines between the categories. For example, BH 176 in the southern part of the Milky Way has properties of both an open and a globular cluster.[107]

In 2005, astronomers discovered a completely new type of star cluster in the Andromeda Galaxy (M31), which is, in several ways, very similar to globular clusters. The new-found clusters contain hundreds of thousands of stars, a similar number to that found in globular clusters. The clusters share other characteristics with globular clusters such as stellar populations and metallicity. What distinguishes them from the globular clusters is that they are much larger – several hundred light-years across – and hundreds of times less dense. The distances between the stars are, therefore, much greater within the newly discovered extended clusters. Parametrically, these clusters lie somewhere between a globular cluster and a dwarf spheroidal galaxy.[108]

The formation of these M31 halo clusters is likely related in some way to accretion.[109] Why M31 has such clusters, while the Milky Way does not, is not yet known. It is also unknown if any other galaxy contains these types of clusters, but it would be very unlikely that M31 is the sole galaxy with extended clusters.[108]

Tidal encounters[edit]

When a globular cluster has a close encounter with a large mass, such as the core region of a galaxy, it undergoes a tidal interaction. The difference in the pull of gravity between the part of the cluster nearest the mass and the pull on the furthest part of the cluster results in a tidal force. A "tidal shock" occurs whenever the orbit of a cluster takes it through the plane of a galaxy.

As a result of a tidal shock, streams of stars can be pulled away from the cluster halo, leaving only the core part of the cluster. These tidal interaction effects create tails of stars that can extend up to several degrees of arc away from the cluster.[110] These tails typically both precede and follow the cluster along its orbit. The tails can accumulate significant portions of the original mass of the cluster, and can form clumplike features.[111]

The globular cluster Palomar 5, for example, is near the apogalactic point of its orbit after passing through the Milky Way. Streams of stars extend outward toward the front and rear of the orbital path of this cluster, stretching out to distances of 13,000 light-years. Tidal interactions have stripped away much of the mass from Palomar 5, and further interactions as it passes through the galactic core are expected to transform it into a long stream of stars orbiting the Milky Way halo.[112]

The Milky Way is in the process of tidally stripping the Sagittarius Dwarf Spheroidal Galaxy of stars and globular clusters through the Sagittarius Stream. As many as 20% of the globular clusters in the Milky Way's outer halo may have originated in that galaxy.[113] Palomar 12, for example, most likely originated in the Sagittarius Dwarf Spheroidal but is now associated with the stream or the Milky way.[114][115] Tidal interactions like these add kinetic energy into a globular cluster, dramatically increasing the evaporation rate and shrinking the size of the cluster.[75] Not only does tidal shock strip off the outer stars from a globular cluster, but the increased evaporation accelerates the process of core collapse.[75][116]

Orbits[edit]

There are many globular clusters with a retrograde orbit round the Milky Way Galaxy.[117] A hypervelocity globular cluster was discovered around Messier 87 in 2014, having a velocity in excess of the escape velocity of M87.[118]

Planets[edit]

Astronomers are searching for exoplanets of stars in globular star clusters.[119] In 2000, the results of a search for giant planets in the globular cluster 47 Tucanae were announced. The lack of any successful discoveries suggests that the abundance of elements (other than hydrogen or helium) necessary to build these planets may need to be at least 40% of the abundance in the Sun. Terrestrial planets are built from heavier elements such as silicon, iron and magnesium. The very low abundance of these elements in globular clusters means that the member stars have a far lower likelihood of hosting Earth-mass planets, when compared with stars in the neighborhood of the Sun. Hence the halo region of the Milky Way galaxy, including globular cluster members, are unlikely to host habitable terrestrial planets.[120]

In spite of the lower likelihood of giant planet formation, just such an object has been found in the globular cluster Messier 4. This planet was detected orbiting a pulsar in the binary star system PSR B1620-26. The eccentric and highly inclined orbit of the planet suggests it may have been formed around another star in the cluster, then was later "exchanged" into its current arrangement.[121] The likelihood of close encounters between stars in a globular cluster can disrupt planetary systems, some of which break free to become rogue planets. Even close orbiting planets can become disrupted, potentially leading to orbital decay and an increase in orbital eccentricity and tidal effects.[122]

See also[edit]

Footnotes[edit]

  1. ^ Omega Centauri was known in antiquity, but Halley discovered its nature as a nebula.
  2. ^ The M before a number refers to Charles Messier's catalogue, while NGC is from the New General Catalogue by John Dreyer.
  3. ^ Harlow Shapley’s error was aggravated by interstellar dust in the Milky Way, which absorbs and diminishes the amount of light from distant objects, such as globular clusters, that reaches the Earth, thus making them appear to be more distant than they are.
  4. ^ The Concentration Class is sometimes given with Arabic numerals (Classes 1–12) rather than Roman numerals.

References[edit]

  1. ^ The Hubble Heritage team (July 1, 1999). "Hubble Images a Swarm of Ancient Stars". HubbleSite News Desk. Space Telescope Science InstituteG. Retrieved May 26, 2006.
  2. ^ a b Harris, William E. (October 1996). "A Catalog of Parameters for Globular Clusters in the Milky Way". The Astronomical Journal. 112: 1487. Bibcode:1996AJ....112.1487H. doi:10.1086/118116. 2010 edition.
  3. ^ Frommert, Hartmut (August 2007). "Milky Way Globular Clusters". Students for the Exploration and Development of Space. Retrieved February 26, 2008.
  4. ^ Camargo, D.; Minniti, D. (2019). "Three candidate globular clusters discovered in the Galactic bulge". Monthly Notices of the Royal Astronomical Society: Letters. 484: L90–L94. arXiv:1901.08574. doi:10.1093/mnrasl/slz010.
  5. ^ Barmby, P.; Huchra, J. P. (2001). "M31 Globular Clusters in the Hubble Space Telescope Archive. I. Cluster Detection and Completeleness". The Astronomical Journal. 122 (5): 2458–2468. arXiv:astro-ph/0107401. Bibcode:2001AJ....122.2458B. doi:10.1086/323457. S2CID 117895577. CS1 maint: discouraged parameter (link)
  6. ^ McLaughlin, Dean E.; Harris, William E.; Hanes, David A. (1994). "The spatial structure of the M87 globular cluster system". Astrophysical Journal. 422 (2): 486–507. Bibcode:1994ApJ...422..486M. doi:10.1086/173744.
  7. ^ Harris, William E. (1991). "Globular cluster systems in galaxies beyond the Local Group". Annual Review of Astronomy and Astrophysics. 29 (1): 543–579. Bibcode:1991ARA&A..29..543H. doi:10.1146/annurev.aa.29.090191.002551.
  8. ^ Lotz, Jennifer M.; Miller, Bryan W.; Ferguson, Henry C. (September 2004). "The Colors of Dwarf Elliptical Galaxy Globular Cluster Systems, Nuclei, and Stellar Halos". The Astrophysical Journal. 613 (1): 262–278. arXiv:astro-ph/0406002. Bibcode:2004ApJ...613..262L. doi:10.1086/422871. S2CID 10800774.
  9. ^ a b Lynn, W.T. (April 1886). "The discovery of the star-cluster 22 Messier in Sagittarius". The Observatory. 9: 163–164. Bibcode:1886Obs.....9..163L.
  10. ^ Halley, Edmond (1716). "An account of several nebualæ or lucid spots like clouds, lately discovered among the fixt stars by help of the telescope". Philosophical Transactions of the Royal Society of London. 29 (347): 390–392. doi:10.1098/rstl.1714.0046.
  11. ^ Patrick Moore (2005). Firefly Atlas of the Universe. Firefly Books. ISBN 978-1-55407-071-8.
  12. ^ Frommert, Hartmut; Kronberg, Christine. "Gottfried Kirch (1639-1710)". Students for the Exploration and Development of Space. Retrieved April 9, 2021.
  13. ^ Plotner, Tammy (May 9, 2016). "Messier 13 (M13) - The Great Hercules Cluster". Universe Today. Retrieved April 23, 2018.
  14. ^ a b Brian Cudnik (September 18, 2012). Faint Objects and How to Observe Them. Springer Science & Business Media. pp. 8–. ISBN 978-1-4419-6756-5.
  15. ^ a b James L. Chen; Adam Chen (July 16, 2015). A Guide to Hubble Space Telescope Objects: Their Selection, Location, and Significance. Springer. pp. 110–. ISBN 978-3-319-18872-0.
  16. ^ Sharp, N. A. "M 22, NGC 6656". NOIRLab. noao-m22. Retrieved August 16, 2006.
  17. ^ Messier (1771). "Catalogue des Nébuleuses & des amas d'Étoiles, que l'on découvre parmi les Étoiles fixes sur l'horizon de Paris; observées à l'Observatoire de la Marine, avec differens instruments" [Catalog of nebulas and star clusters, that one discovers among the fixed stars on the horizon of Paris; observed at the Naval Observatory, with various instruments]. Histoire de l'Académie royale des sciences ... Avec les Mémoires de Mathématique & de Physique, pour la même Année, ... [History of the Royal Academy of Sciences ... with the Mathematical and Physical Memoirs, for the same year, ...] (in French): 435–461. From p. 437: "Le 8 Mai 1764, j'ai découvert une nébuleuse ... de 25d 55′ 40″ méridionale." (On May 8, 1764, I discovered a nebula near Antares, and on its parallel; it is a [source of] light which has little extension, which is dim, and which is seen with difficulty; by using a good telescope to see it, one perceives very small stars in it. Its right ascension was determined to be 242° 16′ 56″, and its declination, 25° 55′ 40″ south.)
  18. ^ Boyd, Richard N. (2008). An introduction to nuclear astrophysics. University of Chicago Press. p. 376. ISBN 978-0-226-06971-5.
  19. ^ Herschel, William (1789). "Catalogue of a second thousand of new nebulæ and clusters of stars, with a few introductory remarks on the construction of the heavens". Philosophical Transactions of the Royal Society of London. 79: 212–255. Bibcode:1789RSPT...79..212H. doi:10.1098/rstl.1789.0021. From p. 218: Discussing the shapes of star clusters, Herschel wrote, "And thus, from the above-mentioned appearances, we come to know that there are globular clusters of stars nearly equal in size, which are scattered evenly at equal distances from the middle, but with an encreasing [sic] accumulation towards the center."
  20. ^ a b Frommert, Hartmut; Kronberg, Christine. "Globular Star Clusters". The Messier Catalog. Students for the Exploration and Development of Space. Archived from the original on April 30, 2015. Retrieved June 19, 2015.
  21. ^ Ashman, Keith M.; Zepf, Stephen E. (1992). "The formation of globular clusters in merging and interacting galaxies". Astrophysical Journal, Part 1. 384: 50–61. Bibcode:1992ApJ...384...50A. doi:10.1086/170850.
  22. ^ a b Ashman, Keith M.; Zepf, Stephen E. (1998). Globular cluster systems. Cambridge astrophysics series. 30. Cambridge University Press. p. 2. ISBN 0-521-55057-2.
  23. ^ Shapley, Harlow (1918). "Globular clusters and the structure of the galactic system". Publications of the Astronomical Society of the Pacific. 30 (173): 42–54. Bibcode:1918PASP...30...42S. doi:10.1086/122686.
  24. ^ Hogg, Helen Battles Sawyer (1965). "Harlow Shapley and Globular Clusters". Publications of the Astronomical Society of the Pacific. 77 (458): 336–346. Bibcode:1965PASP...77..336S. doi:10.1086/128229.
  25. ^ "The Very Large Telescope discovers new kind of globular star cluster". Astronomy. May 13, 2015. Retrieved May 14, 2015.
  26. ^ Piotto, G.; et al. (May 2007). "A Triple Main Sequence in the Globular Cluster NGC 2808". The Astrophysical Journal. 661 (1): L53–L56. arXiv:astro-ph/0703767. Bibcode:2007ApJ...661L..53P. doi:10.1086/518503. S2CID 119376556.
  27. ^ Bastian, Nate; Lardo, Carmela (September 14, 2018). "Multiple Stellar Populations in Globular Clusters". Annual Review of Astronomy and Astrophysics. 56 (1): 83–136. arXiv:1712.01286. Bibcode:2018ARA&A..56...83B. doi:10.1146/annurev-astro-081817-051839. S2CID 59144325.
  28. ^ Piotto, Giampaolo (June 2009). Observations of multiple populations in star clusters. The Ages of Stars, Proceedings of the International Astronomical Union, IAU Symposium. 258. pp. 233–244. arXiv:0902.1422. Bibcode:2009IAUS..258..233P. doi:10.1017/S1743921309031883.
  29. ^ Weaver, D.; Villard, R.; Christensen, L. L.; Piotto, G.; Bedin, L. (May 2, 2007). "Hubble Finds Multiple Stellar 'Baby Booms' in a Globular Cluster". Hubble News Desk. Retrieved May 1, 2007.
  30. ^ Amaro-Seoane, P.; Konstantinidis, S.; Brem, P.; Catelan, M. (2013). "Mergers of multimetallic globular clusters: the role of dynamics". Monthly Notices of the Royal Astronomical Society. 435 (1): 809–821. arXiv:1108.5173. Bibcode:2013MNRAS.435..809A. doi:10.1093/mnras/stt1351. S2CID 54177579.
  31. ^ "This Star Cluster Is Not What It Seems" (Press release). European Southern Observatory. September 10, 2014. eso1428. Retrieved April 7, 2021.
  32. ^ Elmegreen, B. G.; Efremov, Y. N. (1999). "A Universal Formation Mechanism for Open and Globular Clusters in Turbulent Gas". Astrophysical Journal. 480 (2): 235–245. Bibcode:1997ApJ...480..235E. doi:10.1086/303966.
  33. ^ Burkert, Andreas; Tremaine, Scott (April 1, 2010). "A correlation between central supermassive black holes and the globular cluster systems of early-type galaxies". The Astrophysical Journal. 720 (1): 516–521. arXiv:1004.0137. Bibcode:2010ApJ...720..516B. doi:10.1088/0004-637X/720/1/516. S2CID 118632899. A possible explanation is that both large black-hole masses and large globular cluster populations are associated with recent major mergers.
  34. ^ "Young and Exotic Stellar Zoo: ESO's Telescopes Uncover Super Star Cluster in the Milky Way" (Press release). European Southern Observatory. March 22, 2005. eso0510. Archived from the original on April 9, 2007. Retrieved April 7, 2021.
  35. ^ "ESA/Hubble Picture of the Week". Engulfed by Stars Near the Milky Way’s Heart. Retrieved June 28, 2011.
  36. ^ Talpur, Jon (1997). "A Guide to Globular Clusters". Keele University. Retrieved April 25, 2007.
  37. ^ "The Hertzsprung-Russell Diagram of a Globular Cluster". Department of Physics. University of Durham.
  38. ^ a b "Ashes from the Elder Brethren" (Press release). European Southern Observatory. March 2, 2001. eso0107. Retrieved April 7, 2021.
  39. ^ Sigurdsson, Steinn (1992). "Planets in globular clusters?". Astrophysical Journal. 399 (1): L95–L97. Bibcode:1992ApJ...399L..95S. doi:10.1086/186615.
  40. ^ Arzoumanian, Z.; Joshi, K.; Rasio, F. A.; Thorsett, S.E. (1999). "Orbital Parameters of the PSR B1620-26 Triple System". Proceedings of the 160th Colloquium of the International Astronomical Union. 105: 525. arXiv:astro-ph/9605141. Bibcode:1996ASPC..105..525A.
  41. ^ Bekki, K.; Freeman, K.C. (December 2003). "Formation of ω Centauri from an ancient nucleated dwarf galaxy in the young Galactic disc". Monthly Notices of the Royal Astronomical Society. 346 (2): L11–L15. arXiv:astro-ph/0310348. Bibcode:2003MNRAS.346L..11B. doi:10.1046/j.1365-2966.2003.07275.x. S2CID 119466098. CS1 maint: discouraged parameter (link)
  42. ^ Forbes, Duncan A.; Bridges, Terry (January 25, 2010). "Accreted versus in situ Milky Way globular clusters". Monthly Notices of the Royal Astronomical Society. 404 (3): 1203. arXiv:1001.4289. Bibcode:2010MNRAS.404.1203F. doi:10.1111/j.1365-2966.2010.16373.x. S2CID 51825384.
  43. ^ Forbes, Duncan A.; Bastian, Nate; Gieles, Mark; Crain, Robert A.; Kruijssen, J. M. Diederik; Larsen, Søren S.; Ploeckinger, Sylvia; Agertz, Oscar; Trenti, Michele; Ferguson, Annette M. N.; Pfeffer, Joel; Gnedin, Oleg Y. (February 2018). "Globular cluster formation and evolution in the context of cosmological galaxy assembly: open questions". Proceedings of the Royal Society A: Mathematical, Physical and Engineering Sciences. 474 (2210): 20170616. arXiv:1801.05818. Bibcode:2018RSPSA.47470616F. doi:10.1098/rspa.2017.0616. PMC 5832832. PMID 29507511.
  44. ^ "Spot the Difference — Hubble spies another globular cluster, but with a secret". Picture of the Week. ESA/Hubble. Retrieved October 5, 2011.
  45. ^ "APOD: 2021 February 7 – Blue Straggler Stars in Globular Cluster M53". Astronomy Picture of the Day. Retrieved February 28, 2021.
  46. ^ Green, Simon F.; Jones, Mark H.; Burnell, S. Jocelyn (2004). An introduction to the sun and stars. Cambridge University Press. p. 240. ISBN 0-521-54622-2.
  47. ^ a b van Albada, T. S.; Baker, Norman (1973). "On the Two Oosterhoff Groups of Globular Clusters". Astrophysical Journal. 185: 477–498. Bibcode:1973ApJ...185..477V. doi:10.1086/152434.
  48. ^ Buonanno, R.; Corsi, C.E.; Pulone, L. (1995). "ESO 280-SC06". Astronomical Journal. 109: 663. Bibcode:1995AJ....109..663B. doi:10.1086/117309.
  49. ^ Frommert, Hartmut. "Globular cluster ESO 280-S C06, in Ara". Students for the Exploration and Development of Space. Retrieved April 9, 2021.
  50. ^ Harris, W.E. (1976). "Spatial structure of the globular cluster system and the distance to the galactic center". Astronomical Journal. 81: 1095–1116. Bibcode:1976AJ.....81.1095H. doi:10.1086/111991.
  51. ^ Lee, Y.W.; Yoon, S.J. (2002). "On the Construction of the Heavens". An Aligned Stream of Low-Metallicity Clusters in the Halo of the Milky Way. 297 (5581): 578–581. arXiv:astro-ph/0207607. Bibcode:2002Sci...297..578Y. doi:10.1126/science.1073090. PMID 12142530. S2CID 9702759.
  52. ^ a b Leonard, Peter J. T. (1989). "Stellar collisions in globular clusters and the blue straggler problem". The Astronomical Journal. 98: 217–226. Bibcode:1989AJ.....98..217L. doi:10.1086/115138.
  53. ^ a b Rubin, V.C.; Ford, W.K.J. (1999). "A Thousand Blazing Suns: The Inner Life of Globular Clusters". Mercury. 28 (4): 26. Bibcode:1999Mercu..28d..26M. Retrieved June 2, 2006. CS1 maint: discouraged parameter (link)
  54. ^ Savage, D.; Neal, N.; Villard, R.; Johnson, R.; Lebo, H. (September 17, 2002). "Hubble discovers black holes in unexpected places". Space Telescope Science Institute. Retrieved May 25, 2006.
  55. ^ Finley, Dave (May 28, 2007). "Star cluster holds midweight black hole, VLA indicates". NRAO. Retrieved May 29, 2007.
  56. ^ a b Greene, Jenny E.; Strader, Jay; Ho, Luis C. (August 18, 2020). "Intermediate-Mass Black Holes". Annual Review of Astronomy and Astrophysics. 58 (1): 257–312. arXiv:1911.09678. Bibcode:2020ARA&A..58..257G. doi:10.1146/annurev-astro-032620-021835. S2CID 208202069.
  57. ^ Baumgardt, Holger; Hut, Piet; Makino, Junichiro; McMillan, Steve; Portegies Zwart, Simon (2003). "On the Central Structure of M 15". Astrophysical Journal Letters. 582 (1): 21. arXiv:astro-ph/0210133. Bibcode:2003ApJ...582L..21B. doi:10.1086/367537. S2CID 16216186.
  58. ^ Baumgardt, Holger; Hut, Piet; Makino, Junichiro; McMillan, Steve; Portegies Zwart, Simon (2003). "A dynamical model for the globular cluster G 1". Astrophysical Journal Letters. 589 (1): 25. arXiv:astro-ph/0301469. Bibcode:2003ApJ...589L..25B. doi:10.1086/375802. S2CID 119464795. Retrieved September 13, 2006.
  59. ^ Baumgardt, H.; He, C.; Sweet, S. M.; Drinkwater, M.; Sollima, A.; Hurley, J.; Usher, C.; Kamann, S.; Dalgleish, H.; Dreizler, S.; Husser, T. -O. (2019). "No evidence for intermediate-mass black holes in the globular clusters ω Cen and NGC 6624". Monthly Notices of the Royal Astronomical Society. 488 (4): 5340. arXiv:1907.10845. Bibcode:2019MNRAS.488.5340B. doi:10.1093/mnras/stz2060.
  60. ^ "Cosmic fairy lights". ESA/Hubble Picture of the Week. Retrieved April 29, 2014.
  61. ^ Shapley, H. (1917). "Studies based on the colors and magnitudes in stellar clusters. I,II,III". Astrophysical Journal. 45: 118–141. Bibcode:1917ApJ....45..118S. doi:10.1086/142314.
  62. ^ Schwarzschild, Martin (1958). Structure and Evolution of Stars. Princeton University Press. ISBN 0-486-61479-4. CS1 maint: discouraged parameter (link)
  63. ^ Sandage, A. R. (1957). "Observational Approach to Evolution. III. Semiempirical Evolution Tracks for M67 and M3". Astrophysical Journal. 126: 326. Bibcode:1957ApJ...126..326S. doi:10.1086/146405.
  64. ^ Kalirai, J. S.; Richer, H. B. (2010). "Star clusters as laboratories for stellar and dynamical evolution". Philosophical Transactions of the Royal Society of London, Series A. 368 (1913): 755–82. arXiv:0911.0789. Bibcode:2010RSPTA.368..755K. doi:10.1098/rsta.2009.0257. PMID 20083505. S2CID 5561270.
  65. ^ Majaess, D.; Turner, D.; Gieren, W.; Lane, D. (2012). "The Impact of Contaminated RR Lyrae/Globular Cluster Photometry on the Distance Scale". The Astrophysical Journal. 752 (1): L10. arXiv:1205.0255. Bibcode:2012ApJ...752L..10M. doi:10.1088/2041-8205/752/1/L10. S2CID 118528078.
  66. ^ Lee, Jae-Woo; López-Morales, Mercedes; Hong, Kyeongsoo; Kang, Young-Woon; Pohl, Brian L.; Walker, Alistair (2014). "Toward a Better Understanding of the Distance Scale from RR Lyrae Variable Stars: A Case Study for the Inner Halo Globular Cluster NGC 6723". The Astrophysical Journal Supplement Series. 210 (1): 6. arXiv:1311.2054. Bibcode:2014ApJS..210....6L. doi:10.1088/0067-0049/210/1/6. S2CID 119280050.
  67. ^ Hansen, B. M. S.; Brewer, J.; Fahlman, G. G.; Gibson, B. K.; Ibata, R.; Limongi, M.; Rich, R. M.; Richer, H. B.; Shara, M. M.; Stetson, P. B. (2002). "The White Dwarf Cooling Sequence of the Globular Cluster Messier 4". Astrophysical Journal Letters. 574 (2): L155. arXiv:astro-ph/0205087. Bibcode:2002ApJ...574L.155H. doi:10.1086/342528. S2CID 118954762.
  68. ^ Soderblom, David R. (August 2010). "The Ages of Stars". Annual Review of Astronomy and Astrophysics. 48 (1): 581–629. arXiv:1003.6074. Bibcode:2010ARA&A..48..581S. doi:10.1146/annurev-astro-081309-130806.
  69. ^ Chaboyer, Brian (1995). "Absolute ages of globular clusters and the age of the universe". The Astrophysical Journal. 444: L9. arXiv:astro-ph/9412015. Bibcode:1995ApJ...444L...9C. doi:10.1086/187847. S2CID 2416004.
  70. ^ Valcin, David; Bernal, José Luis; Jimenez, Raul; Verde, Licia; Wandelt, Benjamin D. (2020). "Inferring the age of the universe with globular clusters". Journal of Cosmology and Astroparticle Physics. 2020 (12): 002. arXiv:2007.06594. Bibcode:2020JCAP...12..002V. doi:10.1088/1475-7516/2020/12/002. S2CID 220514389.
  71. ^ Majaess, D. (February 23, 2013). "Nearby Ancient Star is Almost as Old as the Universe". Universe Today. Retrieved November 29, 2014.
  72. ^ Staneva, A.; Spassova, N.; Golev, V. (1996). "The Ellipticities of Globular Clusters in the Andromeda Galaxy". Astronomy and Astrophysics Supplement. 116 (3): 447–461. Bibcode:1996A&AS..116..447S. doi:10.1051/aas:1996127.
  73. ^ Hensley, Kerrin (June 20, 2018). "Dating the Evaporation of Globular Clusters". astrobites.
  74. ^ Bose, Sownak; Ginsburg, Idan; Loeb, Abraham (May 23, 2018). "Dating the Tidal Disruption of Globular Clusters with GAIA Data on Their Stellar Streams". The Astrophysical Journal. 859 (1): L13. arXiv:1804.07770. Bibcode:2018ApJ...859L..13B. doi:10.3847/2041-8213/aac48c. S2CID 54514038.
  75. ^ a b c d Benacquista, Matthew J. (2006). "Globular cluster structure". Living Reviews in Relativity. 9 (1): 2. arXiv:astro-ph/0202056. Bibcode:2006LRR.....9....2B. doi:10.12942/lrr-2006-2. PMC 5255526. PMID 28163652.
  76. ^ Baumgardt, H; Hilker, M (August 1, 2018). "A catalogue of masses, structural parameters, and velocity dispersion profiles of 112 Milky Way globular clusters". Monthly Notices of the Royal Astronomical Society. 478 (2): 1520–1557. Bibcode:2018MNRAS.478.1520B. doi:10.1093/mnras/sty1057.
  77. ^ Frenk, C. S.; White, S. D. M. (1980). "The ellipticities of Galactic and LMC globular clusters". Monthly Notices of the Royal Astronomical Society. 286 (3): L39–L42. arXiv:astro-ph/9702024. Bibcode:1997MNRAS.286L..39G. doi:10.1093/mnras/286.3.l39. S2CID 353384.
  78. ^ "Appearances can be deceptive". ESO Picture of the Week. potw1303a. Retrieved February 12, 2013.
  79. ^ Kenneth Janes (November 2000). "Star Clusters" (PDF). Encyclopedia of Astronomy and Astrophysics. p. 2. Retrieved March 26, 2014.
  80. ^ Buonanno, R.; Corsi, C. E.; Buzzoni, A.; Cacciari, C.; Ferraro, F. R.; Fusi Pecci, F. (1994). "The Stellar Population of the Globular Cluster M 3. I. Photographic Photometry of 10 000 Stars". Astronomy and Astrophysics. 290: 69–103. Bibcode:1994A&A...290...69B.
  81. ^ van den Bergh, Sidney (November 2007). "Globular Clusters and Dwarf Spheroidal Galaxies". Monthly Notices of the Royal Astronomical Society. 385 (1): L20–L22. arXiv:0711.4795. Bibcode:2008MNRAS.385L..20V. doi:10.1111/j.1745-3933.2008.00424.x. S2CID 15093329.
  82. ^ Da Costa, G. S.; Freeman, K. C. (May 1976). "The structure and mass function of the globular cluster M3". Astrophysical Journal. 206 (1): 128–137. Bibcode:1976ApJ...206..128D. doi:10.1086/154363.
  83. ^ Brosche, P.; Odenkirchen, M.; Geffert, M. (March 1999). "Instantaneous and average tidal radii of globular clusters". New Astronomy. 4 (2): 133–139. Bibcode:1999NewA....4..133B. doi:10.1016/S1384-1076(99)00014-7.
  84. ^ Djorgovski, S.; King, I. R. (1986). "A preliminary survey of collapsed cores in globular clusters". Astrophysical Journal. 305: L61–L65. Bibcode:1986ApJ...305L..61D. doi:10.1086/184685.
  85. ^ Bianchini, P; Webb, J J; Sills, A; Vesperini, E (March 21, 2018). "Kinematic fingerprint of core-collapsed globular clusters". Monthly Notices of the Royal Astronomical Society: Letters. 475 (1): L96–L100. arXiv:1801.07781. Bibcode:2018MNRAS.475L..96B. doi:10.1093/mnrasl/sly013.
  86. ^ Ashman, Keith M.; Zepf, Stephen E. (1998). Globular cluster systems. Cambridge astrophysics series. 30. Cambridge University Press. p. 29. ISBN 0-521-55057-2.
  87. ^ Binney, James; Merrifield, Michael (1998). Galactic astronomy. Princeton series in astrophysics. Princeton University Press. p. 371. ISBN 0-691-02565-7.
  88. ^ Vanbeveren, D. (2001). The influence of binaries on stellar population studies. Astrophysics and space science library. 264. Springer. p. 397. ISBN 0-7923-7104-6.
  89. ^ Spitzer, L. Jr. (June 2–4, 1986). P. Hut; S. McMillan (eds.). Dynamical Evolution of Globular Clusters. The Use of Supercomputers in Stellar Dynamics, Proceedings of a Workshop Held at the Institute for Advanced Study. 267. Princeton, USA: Springer-Verlag, Berlin Heidelberg New York. p. 3. Bibcode:1986LNP...267....3S. doi:10.1007/BFb0116388.
  90. ^ Gnedin, Oleg Y.; Lee, Hyung Mok; Ostriker, Jeremiah P. (September 1999). "Effects of Tidal Shocks on the Evolution of Globular Clusters". The Astrophysical Journal. 522 (2): 935–949. arXiv:astro-ph/9806245. Bibcode:1999ApJ...522..935G. doi:10.1086/307659. S2CID 11143134.
  91. ^ Bahcall, John N.; Piran, Tsvi; Weinberg, Steven (2004). Dark matter in the universe (2nd ed.). World Scientific. p. 51. ISBN 981-238-841-9.
  92. ^ "The stars of the Large Magellanic Cloud". European Space Agency/Hubble. June 20, 2016. potw1625a. Retrieved April 7, 2021.
  93. ^ "Stellar Sorting in Globular Cluster 47" (Press release). Hubble News Desk. October 4, 2006. 2006-33. Retrieved April 9, 2021.
  94. ^ Secker, Jeff (1992). "A Statistical Investigation into the Shape of the Globular cluster Luminosity Distribution". Astronomical Journal. 104 (4): 1472–1481. Bibcode:1992AJ....104.1472S. doi:10.1086/116332.
  95. ^ Heggie, D. C.; Giersz, M.; Spurzem, R.; Takahashi, K. (1998). Johannes Andersen (ed.). Dynamical Simulations: Methods and Comparisons. Highlights of Astronomy Vol. 11A, as presented at the Joint Discussion 14 of the XXIIIrd General Assembly of the IAU, 1997. Kluwer Academic Publishers. p. 591. arXiv:astro-ph/9711191. Bibcode:1998HiA....11..591H.
  96. ^ Di Cintio, Pierfrancesco; Pasquato, Mario; Simon-Petit, Alicia; Yoon, Suk-Jin (March 3, 2021). "Introducing a new multi-particle collision method for the evolution of dense stellar systems II. Core collapse". arXiv:2103.02424 [astro-ph.GA].
  97. ^ Benacquista, Matthew J. (2006). "Relativistic Binaries in Globular Clusters". Living Reviews in Relativity. 9 (1): 2. Bibcode:2006LRR.....9....2B. doi:10.12942/lrr-2006-2. PMC 5255526. PMID 28163652.
  98. ^ J. Goodman; P. Hut, eds. (1985). Dynamics of Star Clusters (International Astronomical Union Symposia). Springer. ISBN 90-277-1963-2.
  99. ^ Hasani Zonoozi, Akram; et al. (March 2011). "Direct N-body simulations of globular clusters – I. Palomar 14". Monthly Notices of the Royal Astronomical Society. 411 (3): 1989–2001. arXiv:1010.2210. Bibcode:2011MNRAS.411.1989Z. doi:10.1111/j.1365-2966.2010.17831.x. S2CID 54777932.
  100. ^ Yuan, Haibo; Liu, Xiaowei; Xiang, Maosheng; Huang, Yang; Chen, Bingqiu; Wu, Yue; Hou, Yonghui; Zhang, Yong (2015). "Stellar Loci Ii. A Model-Free Estimate of the Binary Fraction for Field FGK Stars". The Astrophysical Journal. 799 (2): 135. arXiv:1412.1233. Bibcode:2015ApJ...799..135Y. doi:10.1088/0004-637X/799/2/135. S2CID 118504277.
  101. ^ Sun, Weijia; De Grijs, Richard; Deng, Licai; Albrow, Michael D. (2021). "Binary-driven stellar rotation evolution at the main-sequence turn-off in star clusters". Monthly Notices of the Royal Astronomical Society. 502 (3): 4350–4358. arXiv:2102.02352. Bibcode:2021MNRAS.502.4350S. doi:10.1093/mnras/stab347.
  102. ^ Duchêne, Gaspard; Kraus, Adam (August 18, 2013). "Stellar Multiplicity". Annual Review of Astronomy and Astrophysics. 51 (1): 269–310. arXiv:1303.3028. Bibcode:2013ARA&A..51..269D. doi:10.1146/annurev-astro-081710-102602. S2CID 119275313.
  103. ^ Giesers, Benjamin; Kamann, Sebastian; Dreizler, Stefan; Husser, Tim-Oliver; Askar, Abbas; Göttgens, Fabian; Brinchmann, Jarle; Latour, Marilyn; Weilbacher, Peter M.; Wendt, Martin; Roth, Martin M. (2019). "A stellar census in globular clusters with MUSE: Binaries in NGC 3201". Astronomy & Astrophysics. 632: A3. arXiv:1909.04050. Bibcode:2019A&A...632A...3G. doi:10.1051/0004-6361/201936203. S2CID 202542401.
  104. ^ Zhou, Yuan; Zhong, Xie Guang (June 1990). "The core evolution of a globular cluster containing massive black holes". Astrophysics and Space Science. 168 (2): 233–241. Bibcode:1990Ap&SS.168..233Y. doi:10.1007/BF00636869. S2CID 122289977.
  105. ^ Pooley, Dave. "Globular Cluster Dynamics: the importance of close binaries in a real N-body system". self-published. Archived from the original on June 19, 2010. Retrieved April 7, 2021.
  106. ^ "Globular Cluster M10". ESA/Hubble Picture of the Week. Retrieved June 18, 2012.
  107. ^ Ortolani, S.; Bica, E.; Barbuy, B. (1995). "BH 176 and AM-2: globular or open clusters?". Astronomy and Astrophysics. 300: 726. Bibcode:1995A&A...300..726O.
  108. ^ a b Huxor, A. P.; Tanvir, N. R.; Irwin, M. J.; R. Ibata (2005). "A new population of extended, luminous, star clusters in the halo of M31". Monthly Notices of the Royal Astronomical Society. 360 (3): 993–1006. arXiv:astro-ph/0412223. Bibcode:2005MNRAS.360.1007H. doi:10.1111/j.1365-2966.2005.09086.x. S2CID 6215035.
  109. ^ Huxor, A. P.; Mackey, A. D.; Ferguson, A. M. N.; Irwin, M. J.; Martin, N. F.; Tanvir, N. R.; Veljanoski, J.; McConnachie, A.; Fishlock, C. K.; Ibata, R.; Lewis, G. F. (August 11, 2014). "The outer halo globular cluster system of M31 – I. The final PAndAS catalogue". Monthly Notices of the Royal Astronomical Society. 442 (3): 2165–2187. doi:10.1093/mnras/stu771.
  110. ^ Lauchner, A.; Wilhelm, R.; Beers, T. C.; Allende Prieto, C. (December 2003). A Search for Kinematic Evidence of Tidal Tails in Globular Clusters. American Astronomical Society Meeting 203, #112.26. Bibcode:2003AAS...20311226L.
  111. ^ Di Matteo, P.; Miocchi, P.; Capuzzo Dolcetta, R. (May 2004). Formation and Evolution of Clumpy Tidal Tails in Globular Clusters. American Astronomical Society, DDA meeting #35, #03.03. Bibcode:2004DDA....35.0303D.
  112. ^ Staude, Jakob (June 3, 2002). "Sky Survey Unveils Star Cluster Shredded By The Milky Way". Image of the Week (Press release). Sloan Digital Sky Survey. Archived from the original on June 29, 2006. Retrieved April 9, 2021.
  113. ^ Carballo-Bello, J. A.; Corral-Santana, J. M.; Martínez-Delgado, D.; Sollima, A.; Muñoz, R. R.; Côté, P.; Duffau, S.; Catelan, M.; Grebel, E. K. (January 24, 2017). "The southern leading and trailing wraps of the Sagittarius tidal stream around the globular cluster Whiting 1". Monthly Notices of the Royal Astronomical Society: Letters. 467 (1): L91–L94. arXiv:1612.08745. Bibcode:2017MNRAS.467L..91C. doi:10.1093/mnrasl/slx006.
  114. ^ Dinescu, D. I.; Majewski, S. R.; Girard, T. M.; Cudworth, K. M. (2000). "The Absolute Proper Motion of Palomar 12: A Case for Tidal Capture from the Sagittarius Dwarf Spheroidal Galaxy". The Astronomical Journal. 120 (4): 1892–1905. arXiv:astro-ph/0006314. Bibcode:2000AJ....120.1892D. doi:10.1086/301552. S2CID 118898193.
  115. ^ Sbordone, L.; Bonifacio, P.; Buonanno, R.; Marconi, G.; Monaco, L.; Zaggia, S. (April 2007). "The exotic chemical composition of the Sagittarius dwarf spheroidal galaxy". Astronomy & Astrophysics. 465 (3): 815–824. arXiv:astro-ph/0612125. Bibcode:2007A&A...465..815S. doi:10.1051/0004-6361:20066385.
  116. ^ Gnedin, Oleg Y.; Ostriker, Jeremiah P. (January 1997). "Destruction of the Galactic Globular Cluster System". The Astrophysical Journal. 474 (1): 223–255. doi:10.1086/303441.
  117. ^ Kravtsov, V. V. (2001). "Globular Clusters and Dwarf Spheroidal Galaxies of the Outer Galactic Halo: on the Putative Scenario of their Formation" (PDF). Astronomical and Astrophysical Transactions. 20 (1): 89–92. Bibcode:2001A&AT...20...89K. doi:10.1080/10556790108208191. Archived from the original (PDF) on February 19, 2009. Retrieved March 2, 2010.
  118. ^ Nelson Caldwell; Jay Strader; Aaron J. Romanowsky; Jean P. Brodie; Ben Moore; Jurg Diemand; Davide Martizzi (February 25, 2014). "A Globular Cluster Toward M87 with a Radial Velocity < -1000 km/s: The First Hypervelocity Cluster". The Astrophysical Journal. 787 (1): L11. arXiv:1402.6319. Bibcode:2014ApJ...787L..11C. doi:10.1088/2041-8205/787/1/L11 (inactive January 14, 2021).CS1 maint: DOI inactive as of January 2021 (link)
  119. ^ Ricard, Elise (January 15, 2016). "Space Friday: Planet Locations, a SUPERnova, and a Black Hole". California Academy of Sciences. Retrieved May 15, 2016.
  120. ^ Gonzalez, Guillermo; Brownlee, Donald; Ward, Peter (July 2001). "The Galactic Habitable Zone: Galactic Chemical Evolution". Icarus. 152 (1): 185–200. arXiv:astro-ph/0103165. Bibcode:2001Icar..152..185G. doi:10.1006/icar.2001.6617. S2CID 18179704.
  121. ^ Sigurdsson, S.; Stairs, I. H.; Moody, K.; Arzoumanian, K. M. Z.; Thorsett, S. E. (2008). "Planets Around Pulsars in Globular Clusters". In Fischer, D.; Rasio, F. A.; Thorsett, S. E.; Wolszczan, A. (eds.). Extreme Solar Systems. ASP Conference Series. 398. p. 119. Bibcode:2008ASPC..398..119S. CS1 maint: discouraged parameter (link)
  122. ^ Spurzem, R.; et al. (May 2009). "Dynamics of Planetary Systems in Star Clusters". The Astrophysical Journal. 697 (1): 458–482. arXiv:astro-ph/0612757. Bibcode:2009ApJ...697..458S. doi:10.1088/0004-637X/697/1/458. S2CID 119083161.

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