Theoretical astronomy

From Wikipedia, the free encyclopedia
Jump to: navigation, search

Based on strict dictionary definitions, "astronomy" refers to "the study of objects and matter outside the Earth's atmosphere and of their physical and chemical properties"[1] In some cases, as in the introduction of the introductory textbook The Physical Universe by Frank Shu, "astronomy" may be used to describe the qualitative study of the subject.[2] Astronomy focuses on celestial objects, space, and the physical universe as a whole. Observations of the Sun, Moon, stars, and planets have formed the basis of timekeeping and navigation.

Astronomy is a branch of science, but unlike other sciences, which have Earth-based laboratories in which controlled experiments are performed, astronomy has its labs located in the heavens far beyond the reach, let alone control, of the terrestrial observer.[3] "So how can one be sure that what one sees out there is subject to the same rules and disciplines of science that govern the local laboratory experiments of physics and chemistry?"[3] "The most incomprehensible thing about the universe is that it is comprehensible." – Albert Einstein.[3]

Ptolemy's Almagest, although a brilliant treatise on theoretical astronomy combined with a practical handbook for computation, nevertheless includes many compromises to reconcile discordant observations. Theoretical astronomy is usually assumed to have begun with Johannes Kepler (1571–1630), and Kepler's laws. It is co-equal with observation. The general history of astronomy deals with the history of the descriptive and theoretical astronomy of the solar system, from the late sixteenth century to the end of the nineteenth century. The major categories of works on the history of modern astronomy include general histories, national and institutional histories, instrumentation, descriptive astronomy, theoretical astronomy, positional astronomy, and astrophysics. Astronomy was early to adopt computational techniques to model stellar and galactic formation and celestial mechanics. From the point of view of theoretical astronomy, not only must the mathematical expression be reasonably accurate but it should preferably exist in a form which is amenable to further mathematical analysis when used in specific problems. Most of theoretical astronomy uses Newtonian theory of gravitation, considering that the effects of general relativity are weak for most celestial objects. The obvious fact is that theoretical astronomy cannot (and does not try) to predict the position, size and temperature of every star in the heavens. Theoretical astronomy by and large has concentrated upon analyzing the apparently complex but periodic motions of celestial objects.

Integrating astronomy and physics[edit]

"Contrary to the belief generally held by laboratory physicists, astronomy has contributed to the growth of our understanding of physics."[3] Physics has helped in the elucidation of astronomical phenomena, and astronomy has helped in the elucidation of physical phenomena:

  1. discovery of the law of gravitation came from the information provided by the motion of the Moon and the planets,
  2. viability of nuclear fusion as demonstrated in the Sun and stars and yet to be reproduced on Earth in a controlled form.[3]

Integrating astronomy with physics involves

Physical interaction Astronomical phenomena
Electromagnetism: observation using the electromagnetic spectrum
black body radiation stellar radiation
synchrotron radiation radio and X-ray sources
inverse-Compton scattering astronomical X-ray sources
acceleration of charged particles pulsars and cosmic rays
absorption/scattering interstellar dust
Strong and weak interaction: nucleosynthesis in stars
cosmic rays
supernovae
primeval universe
Gravity: motion of planets, satellites and binary stars, stellar structure and evolution, N-body motions in clusters of stars and galaxies, black holes, and the expanding universe.[3]

The aim of astronomy is to understand the physics and chemistry from the laboratory that is behind cosmic events so as to enrich our understanding of the cosmos and of these sciences as well.[3]

Integrating astronomy and chemistry[edit]

Astrochemistry, the overlap of the disciplines of astronomy and chemistry, is the study of the abundance and reactions of chemical elements and molecules in space, and their interaction with radiation. The formation, atomic and chemical composition, evolution and fate of molecular gas clouds, is of special interest because it is from these clouds that solar systems form.

Infrared astronomy, for example, has revealed that the interstellar medium contains a suite of complex gas-phase carbon compounds called aromatic hydrocarbons, often abbreviated (PAHs or PACs). These molecules composed primarily of fused rings of carbon (either neutral or in an ionized state) are said to be the most common class of carbon compound in the galaxy. They are also the most common class of carbon molecule in meteorites and in cometary and asteroidal dust (cosmic dust). These compounds, as well as the amino acids, nucleobases, and many other compounds in meteorites, carry deuterium and isotopes of carbon, nitrogen, and oxygen that are very rare on earth, attesting to their extraterrestrial origin. The PAHs are thought to form in hot circumstellar environments (around dying carbon rich red giant stars).

The sparseness of interstellar and interplanetary space results in some unusual chemistry, since symmetry-forbidden reactions cannot occur except on the longest of timescales. For this reason, molecules and molecular ions which are unstable on Earth can be highly abundant in space, for example the H3+ ion. Astrochemistry overlaps with astrophysics and nuclear physics in characterizing the nuclear reactions which occur in stars, the consequences for stellar evolution, as well as stellar 'generations'. Indeed, the nuclear reactions in stars produce every naturally occurring chemical element. As the stellar 'generations' advance, the mass of the newly formed elements increases. A first-generation star uses elemental hydrogen (H) as a fuel source and produces helium (He). Hydrogen is the most abundant element, and it is the basic building block for all other elements as its nucleus has only one proton. Gravitational pull toward the center of a star creates massive amounts of heat and pressure, which cause nuclear fusion. Through this process of merging nuclear mass, heavier elements are formed. Lithium, carbon, nitrogen and oxygen are examples of elements that form in stellar fusion. After many stellar generations, very heavy elements are formed (e.g. iron and lead).

Tools of theoretical astronomy[edit]

Theoretical astronomers use a wide variety of tools which include analytical models (for example, polytropes to approximate the behaviors of a star) and computational numerical simulations. Each has some advantages. Analytical models of a process are generally better for giving insight into the heart of what is going on. Numerical models can reveal the existence of phenomena and effects that would otherwise not be seen.[4][5]

Astronomy theorists endeavor to create theoretical models and figure out the observational consequences of those models. This helps observers look for data that can refute a model or help in choosing between several alternate or conflicting models.

Theorists also try to generate or modify models to take into account new data. Consistent with the general scientific approach, in the case of an inconsistency, the general tendency is to try to make minimal modifications to the model to fit the data. In some cases, a large amount of inconsistent data over time may lead to total abandonment of a model.

Topics of theoretical astronomy[edit]

Topics studied by theoretical astronomers include:

  1. stellar dynamics and evolution;
  2. galaxy formation;
  3. large-scale structure of matter in the Universe;
  4. origin of cosmic rays;
  5. general relativity and physical cosmology, including string cosmology and astroparticle physics.

Astrophysical relativity serves as a tool to gauge the properties of large scale structures for which gravitation plays a significant role in physical phenomena investigated and as the basis for black hole (astro)physics and the study of gravitational waves.

Astronomical models[edit]

Some widely accepted and studied theories and models in astronomy, now included in the Lambda-CDM model are the Big Bang, Cosmic inflation, dark matter, and fundamental theories of physics.

A few examples of this process:

Physical process Experimental tool Theoretical model Explains/predicts
Gravitation Radio telescopes Self-gravitating system Emergence of a star system
Nuclear fusion Spectroscopy Stellar evolution How the stars shine and how metals formed
The Big Bang Hubble Space Telescope, COBE Expanding universe Age of the Universe
Quantum fluctuations Cosmic inflation Flatness problem
Gravitational collapse X-ray astronomy General relativity Black holes at the center of Andromeda galaxy
CNO cycle in stars

Leading topics in theoretical astronomy[edit]

Dark matter and dark energy are the current leading topics in astronomy,[6] as their discovery and controversy originated during the study of the galaxies.

Theoretical astrophysics[edit]

Of the topics approached with the tools of theoretical physics, particular consideration is often given to stellar photospheres, stellar atmospheres, the solar atmosphere, planetary atmospheres, gaseous nebulae, nonstationary stars, and the interstellar medium. Special attention is given to the internal structure of stars.[7]

Weak equivalence principle[edit]

The observation of a neutrino burst within 3 h of the associated optical burst from Supernova 1987A in the Large Magellanic Cloud (LMC) gave theoretical astrophysicists an opportunity to test that neutrinos and photons follow the same trajectories in the gravitational field of the galaxy.[8]

Thermodynamics for stationary black holes[edit]

A general form of the first law of thermodynamics for stationary black holes can be derived from the microcanonical functional integral for the gravitational field.[9] The boundary data

  1. the gravitational field as described with a micocanonical system in a spatially finite region and
  2. the density of states expressed formally as a functional integral over Lorentzian metrics and as a functional of the geometrical boundary data that are fixed in the corresponding action,

are the thermodynamical extensive variables, including the energy and angular momentum of the system.[9] For the simpler case of nonrelativistic mechanics as is often observed in astrophysical phenomena associated with a black hole event horizon, the density of states can be expressed as a real-time functional integral and subsequently used to deduce Feynman's imaginary-time functional integral for the canonical partition function.[9]

Theoretical astrochemistry[edit]

Reaction equations and large reaction networks are an important tool in theoretical astrochemistry, especially as applied to the gas-grain chemistry of the interstellar medium.[10] Theoretical astrochemistry offers the prospect of being able to place constraints on the inventory of organics for exogenous delivery to the early Earth.

Interstellar organics[edit]

"An important goal for theoretical astrochemistry is to elucidate which organics are of true interstellar origin, and to identify possible interstellar precursors and reaction pathways for those molecules which are the result of aqueous alterations."[11] One of the ways this goal can be achieved is through the study of carbonaceous material as found in some meteorites. Carbonaceous chondrites (such as C1 and C2) include organic compounds such as amines and amides; alcohols, aldehydes, and ketones; aliphatic and aromatic hydrocarbons; sulfonic and phosphonic acids; amino, hydroxycarboxylic, and carboxylic acids; purines and pyrimidines; and kerogen-type material.[11] The organic inventories of primitive meteorites display large and variable enrichments in deuterium, 13C and 15N which is indicative of their retention of an interstellar heritage.[11]

Chemistry in cometary comae[edit]

The chemical composition of comets should reflect both the conditions in the outer solar nebula some 4.5 x 109 ayr, and the nature of the natal interstellar cloud from which the Solar system was formed.[12] While comets retain a strong signature of their ultimate interstellar origins, significant processing must have occurred in the protosolar nebula.[12] Early models of coma chemistry showed that reactions can occur rapidly in the inner coma, where the most important reactions are proton transfer reactions.[12] Such reactions can potentially cycle deuterium between the different coma molecules, altering the initial D/H ratios released from the nuclear ice, and necessitating the construction of accurate models of cometary deuterium chemistry, so that gas-phase coma observations can be safely extrapolated to give nuclear D/H ratios.[12]

Theoretical chemical astronomy[edit]

While the lines of conceptual understanding between theoretical astrochemistry and theoretical chemical astronomy often become blurred so that the goals and tools are the same, there are subtle differences between the two sciences. Theoretical chemistry as applied to astronomy seeks to find new ways to observe chemicals in celestial objects, for example. This often leads to theoretical astrochemistry having to seek new ways to describe or explain those same observations.

Astronomical spectroscopy[edit]

The new era of chemical astronomy had to await the clear enunciation of the chemical principles of spectroscopy and the applicable theory.[13]

Chemistry of dust condensation[edit]

Supernova radioactivity dominates light curves and the chemistry of dust condensation is also dominated by radioactivity.[14] Dust is usually either carbon or oxides depending on which is more abundant, but Compton electrons dissociate the CO molecule in about one month.[14] The new chemical astronomy of supernova solids depends on the supernova radioactivity:

  1. the radiogenesis of 44Ca from 44Ti decay after carbon condensation establishes their supernova source,
  2. their opacity suffices to shift emission lines blueward after 500 d and emits significant infrared luminosity,
  3. parallel kinetic rates determine trace isotopes in meteoritic supernova graphites,
  4. the chemistry is kinetic rather than due to thermal equilibrium and
  5. is made possible by radiodeactivation of the CO trap for carbon.[14]

Theoretical physical astronomy[edit]

Like theoretical chemical astronomy, the lines of conceptual understanding between theoretical astrophysics and theoretical physical astronomy are often blurred, but, again, there are subtle differences between these two sciences. Theoretical physics as applied to astronomy seeks to find new ways to observe physical phenomena in celestial objects and what to look for, for example. This often leads to theoretical astrophysics having to seek new ways to describe or explain those same observations, with hopefully a convergence to improve our understanding of the local environment of Earth and the physical Universe.

Weak interaction and nuclear double beta decay[edit]

Nuclear matrix elements of relevant operators as extracted from data and from a shell-model and theoretical approximations both for the two-neutrino and neutrinoless modes of decay are used to explain the weak interaction and nuclear structure aspects of nuclear double beta decay.[15]

Neutron-rich isotopes[edit]

New neutron-rich isotopes, 34Ne, 37Na, and 43Si have been produced unambiguously for the first time, and convincing evidence for the particle instability of three others, 33Ne, 36Na, and 39Mg has been obtained.[16] These experimental findings compare with recent theoretical predictions.[16]

Theory of astronomical time keeping[edit]

Until recently all the time units that appear natural to us are caused by astronomical phenomena:

  1. Earth's orbit around the Sun => the year, and the seasons,
  2. Moon's orbit around the Earth => the month,
  3. Earth's rotation and the succession of brightness and darkness => the day (and night).

High precision appears problematic:

  1. amibiguities arise in the exact definition of a rotation or revolution,
  2. some astronomical processes are uneven and irregular, such as the noncommensurability of year, month, and day,
  3. there are a multitude of time scales and calendars to solve the first two problems.[17]

Some of these time scales are sidereal time, solar time, and universal time.

Atomic time[edit]

Historical accuracy of atomic clocks from NIST.

From the Systeme Internationale (SI) comes the second as defined by the duration of 9 192 631 770 cycles of a particular hyperfine structure transition in the ground state of 133Cesium.[17] For practical usability a device is required that attempts to produce the SI second (s) such as an atomic clock. But not all such clocks agree. The weighted mean of many clocks distributed over the whole Earth defines the Temps Atomique International; i.e., the Atomic Time TAI.[17] From the General theory of relativity the time measured depends on the altitude on Earth and the spatial velocity of the clock so that TAI refers to a location on sea level that rotates with the Earth.[17]

Ephemeris time[edit]

Since the Earth's rotation is irregular, any time scale derived from it such as Greenwich Mean Time led to recurring problems in predicting the Ephemerides for the positions of the Moon, Sun, planets and their natural satellites.[17] In 1976 the International Astronomical Union (IAU) resolved that the theoretical basis for ephemeris time (ET) was wholly non-relativistic, and therefore, beginning in 1984 ephemeris time would be replaced by two further time scales with allowance for relativistic corrections. Their names, assigned in 1979,[18] emphasized their dynamical nature or origin, Barycentric Dynamical Time (TDB) and Terrestrial Dynamical Time (TDT). Both were defined for continuity with ET and were based on what had become the standard SI second, which in turn had been derived from the measured second of ET.

During the period 1991–2006, the TDB and TDT time scales were both redefined and replaced, owing to difficulties or inconsistencies in their original definitions. The current fundamental relativistic time scales are Geocentric Coordinate Time (TCG) and Barycentric Coordinate Time (TCB). Both of these have rates that are based on the SI second in respective reference frames (and hypothetically outside the relevant gravity well), but due to relativistic effects, their rates would appear slightly faster when observed at the Earth's surface, and therefore diverge from local Earth-based time scales using the SI second at the Earth's surface.[19]

The currently defined IAU time scales also include Terrestrial Time (TT) (replacing TDT, and now defined as a re-scaling of TCG, chosen to give TT a rate that matches the SI second when observed at the Earth's surface),[20] and a redefined Barycentric Dynamical Time (TDB), a re-scaling of TCB to give TDB a rate that matches the SI second at the Earth's surface.

Extraterrestrial time-keeping[edit]

Stellar dynamical time scale[edit]

For a star, the dynamical time scale is defined as the time that would be taken for a test particle released at the surface to fall under the star's potential to the centre point, if pressure forces were negligible. In other words, the dynamical time scale measures the amount of time it would take a certain star to collapse in the absence of any internal pressure. By appropriate manipulation of the equations of stellar structure this can be found to be

 \tau_{dynamical} \simeq \frac{R}{v} = \sqrt{\frac{R^3}{2GM}} \sim 1/\sqrt{G\rho}

where R is the radius of the star, G is the gravitational constant, M is the mass of the star and v is the escape velocity. As an example, the Sun dynamical time scale is approximately 1133 seconds. Note that the actual time it would take a star like the Sun to collapse is greater because internal pressure is present.

The 'fundamental' oscillatory mode of a star will be at approximately the dynamical time scale. Oscillations at this frequency are seen in Cepheid variables.

Theory of astronomical navigation[edit]

On Earth[edit]

The basic characteristics of applied astronomical navigation are

  1. usable in all areas of sailing around the Earth,
  2. applicable autonomously (does not depend on others – persons or states) and passively (does not emit energy),
  3. conditional usage via optical visibility (of horizon and celestial bodies), or state of cloudiness,
  4. precisional measurement, sextant is 0.1', altitude and position is between 1.5' and 3.0'.
  5. temporal determination takes a couple of minutes (using the most modern equipment) and ≤ 30 min (using classical equipment).[21]

The superiority of satellite navigation systems to astronomical navigation are currently undeniable, especially with the development and use of GPS/NAVSTAR.[21] This global satellite system

  1. enables automated three-dimensional positioning at any moment,
  2. automatically determines position continuously (every second or even more often),
  3. determines position independent of weather conditions (visibility and cloudiness),
  4. determines position in real time to a few meters (two carrying frequencies) and 100 m (modest commercial receivers), which is two to three orders of magnitude better than by astronomical observation,
  5. is simple even without expert knowledge,
  6. is relatively cheap, comparable to equipment for astronomical navigation, and
  7. allows incorporation into integrated and automated systems of control and ship steering.[21] The use of astronomical or celestial navigation is disappearing from the surface and beneath or above the surface of the Earth.

Geodetic astronomy is the application of astronomical methods into networks and technical projects of geodesy for

Astronomical algorithms are the algorithms used to calculate ephemerides, calendars, and positions (as in celestial navigation or satellite navigation).

Many astronomical and navigational computations use the Figure of the Earth as a surface representing the Earth.

The International Earth Rotation and Reference Systems Service (IERS), formerly the International Earth Rotation Service, is the body responsible for maintaining global time and reference frame standards, notably through its Earth Orientation Parameter (EOP) and International Celestial Reference System (ICRS) groups.

Deep space[edit]

The Deep Space Network, or DSN, is an international network of large antennas and communication facilities that supports interplanetary spacecraft missions, and radio and radar astronomy observations for the exploration of the solar system and the universe. The network also supports selected Earth-orbiting missions. DSN is part of the NASA Jet Propulsion Laboratory (JPL).

Aboard an exploratory vehicle[edit]

An observer becomes a deep space explorer upon escaping Earth's orbit.[22] While the Deep Space Network maintains communication and enables data download from an exploratory vessel, any local probing performed by sensors or active systems aboard usually require astronomical navigation, since the enclosing network of satellites to ensure accurate positioning is absent.

See also[edit]

References[edit]

  1. ^ "Merriam-Webster Online". Results for "astronomy". Retrieved 2007-06-20. 
  2. ^ Shu FH (1982). The Physical Universe. Mill Valley, California: University Science Books. ISBN 0-935702-05-9. 
  3. ^ a b c d e f g Narlikar JV (1990). Pasachoff JM, Percy JR, ed. Curriculum for the Training of Astronomers ‘’In: The Teaching of astronomy. Cambridge, England: Cambridge University Press. 
  4. ^ Roth H (1932). "A Slowly Contracting or Expanding Fluid Sphere and its Stability". Phys. Rev. 39 (3): 525–9. Bibcode:1932PhRv...39..525R. doi:10.1103/PhysRev.39.525. 
  5. ^ Eddington AS (1926). Internal Constitution of the Stars. Cambridge, England: Cambridge University Press. ISBN 0-521-33708-9. 
  6. ^ http://imagine.gsfc.nasa.gov/docs/science/know_l1/dark_matter.html third paragraph, "There is currently much ongoing research by scientists attempting to discover exactly what this dark matter is". Retrieved 2009-11-02
  7. ^ Sobolev VV (1985). Course in theoretical astrophysics (3rd revised and enlarged ed.). Moscow: Izdatel'stvo Nauka. p. 504. 
  8. ^ Krauss LM, Tremaine S (Mar 1988). "Test of the Weak Equivalence Principle for Neutrinos and Photons". Phys. Rev. Lett. 60 (3): 176–7. Bibcode:1988PhRvL..60..176K. doi:10.1103/PhysRevLett.60.176. 
  9. ^ a b c Brown JD, York JW Jr (Apr 1993). "Microcanonical functional integral for the gravitational field". Phys. Rev. D 47 (4): 1420–31. arXiv:gr-qc/9209014. Bibcode:1993PhRvD..47.1420B. doi:10.1103/PhysRevD.47.1420. 
  10. ^ Vasyunin AI, Semenov DA, Wiebe DS, Henning T (Feb 2009). "A UNIFIED MONTE CARLO TREATMENT OF GAS-GRAIN CHEMISTRY FOR LARGE REACTION NETWORKS. I. TESTING VALIDITY OF RATE EQUATIONS IN MOLECULAR CLOUDS". Ap J. 691 (2): 1459–69. arXiv:0810.1591. Bibcode:2009ApJ...691.1459V. doi:10.1088/0004-637X/691/2/1459. 
  11. ^ a b c Ehrenfreund P, Charnley SB, Botta O (2005). Livio M, Reid IN, Sparks WB, ed. A voyage from dark clouds to the early Earth In: Astrophysics of life: proceedings of the Space Telescope Science Institute Symposium held in Baltimore, Maryland, May 6–9, 2002, Volume 16 of Space Telescope Science Institute symposium series. Cambridge, England: Cambridge University Press. pp. 1–20 of 110. ISBN 9780521824903. 
  12. ^ a b c d Rodgers SD, Charnley SB (Mar 2002). "A model of the chemistry in cometary comae: deuterated molecules". Monthly Notices of the Royal Astronomical Society (MNRAS). 330 (3): 660–74. Bibcode:2002MNRAS.330..660R. doi:10.1046/j.1365-8711.2002.05165.x. 
  13. ^ Merrill PW (1954). "Great Epochs in Astronomy". Astronomical Soc Pac Leaf. 7: 41–8. Bibcode:1954ASPL....7...41M. 
  14. ^ a b c Clayton DD, Liu W (1999). "Radioactivity Frontier for Supernova Chemistry". Bull Am Astron Soc. 31: 739. Bibcode:1999HEAD....4.3602C. 
  15. ^ Suhonen J, Civitarese O (Jul 1998). "Weak-interaction and nuclear-structure aspects of nuclear double beta decay". Phys Rep. 300 (3): 123–214. doi:10.1016/S0370-1573(97)00087-2. 
  16. ^ a b Notani M, Sakurai H, Aoi N, Yanagisawa Y, Saito A, Imai N, Gomi T, Miura M, Michimasa S, Iwasaki H, Fukuda N, Ishihara M, Kubo T, Kubono S, Kumagai H, Lukyanov SM, Motobayashi T, Onishi TK, Penionzhkevich YE, Shimoura S, Teranishi T, Ue K, Ugryumov V, Yoshida A (Aug 2002). "New neutron-rich isotopes, 34Ne, 37Na and 43Si, produced by fragmentation of a 64 A MeV 48Ca beam". Phys. Lett. B 542 (1): 49–54. Bibcode:2002PhLB..542...49N. doi:10.1016/S0370-2693(02)02337-7. 
  17. ^ a b c d e Husfeld D, Kronberg C. "Astronomical Time Keeping". 
  18. ^ Guinot B, Seidelmann PK (Apr 1988). "Time scales – Their history, definition and interpretation". Astronomy and Astrophysics 194 (1-2): 304–8. Bibcode:1988A&A...194..304G. 
  19. ^ Klioner S et al. (2009). "Units of relativistic time scales and associated quantities". IAU Symposium 261. 
  20. ^ "IAU 2000 resolutions, at Resolution B1.9.". 
  21. ^ a b c Stajic D (Oct 2003). "Astronomical navigation at the beginning of the third millenium". Publ Astron Obs Belgrade In: Proceedings of the XIII National Conference of Yugoslav Astronomers, Belgrade, October 17–20, 2002 75: 209–16. Bibcode:2003POBeo..75..209S.  [sic]
  22. ^ Kawakatsu Y (Dec 2007). "Concept study on Deep Space Orbit Transfer Vehicle". Acta Astronaut. 61 (11-12): 1019–28. Bibcode:2007AcAau..61.1019K. doi:10.1016/j.actaastro.2006.12.019. 

External links[edit]