Barnard's Star // is a very low-mass red dwarf star about six light-years away from Earth in the constellation of Ophiuchus, the Snake-holder. Barnard's Star is the fourth-closest known individual star to the Sun, after the three components of the Alpha Centauri system, and the closest star in the Northern Hemisphere. Despite its proximity, Barnard's Star, at a dim apparent magnitude of about nine, is not visible with the unaided eye; however, it is much brighter in the infrared than it is in visible light. The star is named for American astronomer E.E. Barnard. He was not the first to observe the star (it appeared on Harvard College University plates in 1888 and 1890), but in 1916 he measured its proper motion as 10.3 arcseconds (20,000 inverse radians) per year, which remains the largest-known proper motion of any star relative to the Solar System.
Barnard's Star has been the subject of much study, and it has probably received more attention from astronomers than any other class M dwarf star due to its proximity and favorable location for observation near the celestial equator. Historically, research on Barnard's Star has focused on measuring its stellar characteristics, its astrometry, and also refining the limits of possible extrasolar planets. Although Barnard's Star is an ancient star, some observations suggest that it still experiences star flare events.
Barnard's Star has also been the subject of some controversy. For a decade, from the early 1960s to the early 1970s, Peter van de Kamp claimed that there were one or more gas giants in orbit around it. Although the presence of small terrestrial planets around Barnard's Star remains a possibility, Van de Kamp's specific claims of large gas giants were refuted in the mid-1970s.
In approximately 10,000 years the NASA probe Pioneer 10 will pass within 3.8 light years of the star. However, no information will be gained by the event as both Pioneer probes exhausted their power supplies in the early 2000s.
Barnard's Star is a red dwarf of the dim spectral type M4, and it is too faint to see without a telescope. Its apparent magnitude is 9.54. This compares with a magnitude of −1.5 for Sirius – the brightest star in the night sky – and about 6.0 for the faintest visible objects with the naked eye (this magnitude scale is logarithmic, and so the magnitude of 9.54 is only about 1/27th of the brightness of the faintest star that can be seen with the naked eye under good viewing conditions).
At seven to 12 billion years of age, Barnard's Star is considerably older than the Sun [4.567 billion], and it might be among the oldest stars in the Milky Way galaxy. Barnard's Star has lost a great deal of rotational energy, and the periodic slight changes in its brightness indicate that it rotates just once in 130 days (the Sun rotates in 25). Given its age, Barnard's Star was long assumed to be quiescent in terms of stellar activity. However in 1998, astronomers observed an intense stellar flare, surprisingly showing that Barnard's Star is a flare star. Barnard's Star has the variable star designation V2500 Ophiuchi. In 2003, Barnard's Star presented the first detectable change in the radial velocity of a star caused by its motion. Further variability in the radial velocity of Barnard's Star was attributed to its stellar activity.
The proper motion of Barnard's Star corresponds to a relative lateral speed ("sideways" relative to our line of sight to the Sun) of 90 km/s. The 10.3 seconds of arc it travels annually amounts to a quarter of a degree in a human lifetime, roughly half the angular diameter of the full Moon.
The radial velocity of Barnard's Star towards the Sun can be measured by its blue shift. Two measurements are given in catalogues: 106.8 km/s in SIMBAD, which refers to a 1967 compilation of older measurements, and 110.8 km/s in ARICNS and similar values in all modern astronomical references. These measurements, combined with proper motion, suggest a true velocity relative to the Sun of 139.7 and 142.7 km/s, respectively. Barnard's Star will make its closest approach to the Sun around AD 11,800, when it approaches to within about 3.75 light-years. However, at that time, Barnard's Star will not be the nearest star, since Proxima Centauri will have moved even closer to the Sun. Barnard's Star will still be too dim to be seen with the naked eye at the time of its closest approach, since its apparent magnitude will be about 8.5 then. After that it will gradually recede from the Sun.
Barnard's Star has approximately 14% of a solar mass (M☉), and it has a radius 15% to 20% of that of the Sun. In 2003, its radius was estimated as 0.20±0.008 of the solar radius, at the high end of the ranges that were typically calculated in the past, indicating that previous estimates of the radius of Barnard's Star probably underestimated the actual value. Thus, although Barnard's Star has roughly 150 times the mass of Jupiter (MJ), its radius is only 1.5 to 2.0 times larger, reflecting the tendency of objects in the brown dwarf range to be about the same size. Its effective temperature is 3,134(±102) kelvin, and it has a visual luminosity just 4/10,000ths of solar luminosity, corresponding to a bolometric luminosity of 34.6/10,000ths. Barnard's Star is so faint that if it were at the same distance from Earth as the Sun is, it would appear only 100 times brighter than a full moon, comparable to the brightness of the Sun at 80 Astronomical Units.
In a broad survey of the metallicity of M-class dwarf stars, Barnard's Star's was placed between −0.5 and −1.0 on the metallicity scale, which is roughly 10 to 32% of the value for the Sun. Metallicity, the proportion of stellar mass made up of elements heavier than helium, helps classify stars relative to the galactic population. Barnard's Star seems to be typical of the old, red dwarf population II stars, yet these are also generally metal-poor halo stars. While sub-solar, Barnard's Star's metallicity is higher than a halo star and is in keeping with the low end of the metal-rich disk star range; this, plus its high space motion, have led to the designation "Intermediate Population II star", between a halo and disk star.
Barnard's Star distance estimates
|Source||Parallax, mas||Distance, pc||Distance, ly||Ref.|
|Woolley et al. (1970)||548 ± 3||1.825 ± 0.01||5.95 ± 0.03|||
|Gliese & Jahreiß (1991)||545.3 ± 1.0||1.834 ± 0.003||5.981 ± 0.011|||
|van Altena et al. (1995)||545.6 ± 1.3||1.833 ± 0.004||5.978 ± 0.014|||
|Perryman et al. (1997)
|549.01 ± 1.58||1.821 ± 0.005||5.941 ± 0.017|||
|Perryman et al. (1997)
|Benedict et al. (1999)||545.4 ± 0.3||1.8335 ± 0.001||5.98 ± 0.003|||
|van Leeuwen (2007)||548.31 ± 1.51||1.824 ± 0.005||5.948 ± 0.016|||
|RECONS TOP100 (2012)||545.51 ± 0.29[nb 1]||1.8331 ± 0.001||5.979 ± 0.003|||
|Dittmann et al. (2014)||547.40 ± 8.40||1.827 ± 0.028||5.96 ± 0.09|||
Non-trigonometric distance estimates are marked in italic. The best estimate is marked in bold.
Claims of a planetary system
For a decade from 1963 to about 1973, a substantial number of astronomers accepted a claim by Peter van de Kamp that he had detected, by using astrometry, a perturbation in the proper motion of Barnard's Star consistent with its having one or more planets comparable in mass with Jupiter. Van de Kamp had been observing the star from 1938, attempting, with colleagues at the Swarthmore College observatory, to find minuscule variations of one micrometre in its position on photographic plates consistent with orbital perturbations (wobbles) in the star that would indicate a planetary companion; this involved as many as ten people averaging their results in looking at plates, to avoid systemic, individual errors. Van de Kamp's initial suggestion was a planet having about 1.6 MJ at a distance of 4.4 AU in a slightly eccentric orbit, and these measurements were apparently refined in a 1969 paper. Later that year, Van de Kamp suggested that there were two planets of 1.1 and 0.8 MJ.
Other astronomers subsequently repeated Van de Kamp's measurements, and two important papers in 1973 undermined the claim of a planet or planets. George Gatewood and Heinrich Eichhorn, at a different observatory and using newer plate measuring techniques, failed to verify the planetary companion. Another paper published by John L. Hershey four months earlier, also using the Swarthmore observatory, found that changes in the astrometric field of various stars correlated to the timing of adjustments and modifications that had been carried out on the refractor telescope's objective lens; the planetary "discovery" was an artifact of maintenance and upgrade work. The affair has been discussed as part of a broader scientific review.
Van de Kamp never acknowledged any error and published a further confirmation of two planets' existence as late as 1982; he died in 1995. Wulff Heintz, Van de Kamp's successor at Swarthmore and an expert on double stars, questioned his findings and began publishing criticisms from 1976 onwards. The two men were reported to have become estranged from each other because of this.
Refining planetary boundaries
While not completely ruling out the possibility of planets, null results for planetary companions continued throughout the 1980s and 1990s, the latest based on interferometric work with the Hubble Space Telescope in 1999. By refining the values of a star's motion, the mass and orbital boundaries for possible planets are tightened: in this way astronomers are often able to describe what types of planets cannot orbit a given star.
M dwarfs such as Barnard's Star are more easily studied than larger stars in this regard because their lower masses render perturbations more obvious. Gatewood was thus able to show in 1995 that planets with 10 MJ (the lower limit for brown dwarfs) were impossible around Barnard's Star, in a paper which helped refine the negative certainty regarding planetary objects in general. In 1999, work with the Hubble Space Telescope further excluded planetary companions of 0.8 MJ with an orbital period of less than 1,000 days (Jupiter's orbital period is 4,332 days), while Kuerster determined in 2003 that within the habitable zone around Barnard's Star, planets are not possible with an "M sin i" value greater than 7.5 times the mass of the Earth (M⊕), or with a mass greater than 3.1 times the mass of Neptune (much lower than van de Kamp's smallest suggested value).
Even though this research has greatly restricted the possible properties of planets around Barnard's Star, it has not ruled them out completely; terrestrial planets would be difficult to detect. NASA's Space Interferometry Mission, which was to begin searching for extrasolar Earth-like planets, was reported to have chosen Barnard's Star as an early search target. However, this mission was shut down in 2010. ESA's similar Darwin interferometry mission had the same goal, but was stripped of funding in 2007.
Excepting the planet controversy, the best known study of Barnard's Star was part of Project Daedalus. Undertaken between 1973 and 1978, it suggested that rapid, unmanned travel to another star system is possible with existing or near-future technology. Barnard's Star was chosen as a target, partly because it was believed to have planets.
The theoretical model suggested that a nuclear pulse rocket employing nuclear fusion (specifically, electron bombardment of deuterium and helium-3) and accelerating for four years could achieve a velocity of 12% of the speed of light. The star could then be reached in 50 years, within a human lifetime. Along with detailed investigation of the star and any companions, the interstellar medium would be examined and baseline astrometric readings performed.
The initial Project Daedalus model sparked further theoretical research. In 1980, Robert Freitas suggested a more ambitious plan: a self-replicating spacecraft intended to search for and make contact with extraterrestrial life. Built and launched in Jovian orbit, it would reach Barnard's Star in 47 years under parameters similar to those of the original Project Daedalus. Once at the star, it would begin automated self-replication, constructing a factory, initially to manufacture exploratory probes and eventually to create a copy of the original spacecraft after 1,000 years.
The flare in 1998
The observation of a stellar flare on Barnard's Star has added another element of interest to its study. Noted by William Cochran, University of Texas at Austin, based on changes in the spectral emissions on July 17, 1998 (during an unrelated search for planetary "wobbles"), it was four more years before the flare was fully analyzed. At that point Diane Paulson et al., now of Goddard Space Flight Center, suggested that the flare's temperature was 8000 K, more than twice the normal temperature of the star, although simply analyzing the spectra cannot precisely determine the flare's total output. Given the essentially random nature of flares, she noted "the star would be fantastic for amateurs to observe".
The flare was surprising because intense stellar activity is not expected around stars of such age. Flares are not completely understood, but are believed to be caused by strong magnetic fields which suppress plasma convection and lead to sudden outbursts: strong magnetic fields occur in rapidly rotating stars, while old stars tend to rotate slowly. An event of such magnitude around Barnard's Star is thus presumed to be a rarity. Research on the star's periodicity, or changes in stellar activity over a given timescale, also suggest it ought to be quiescent; 1998 research showed weak evidence for periodic variation in Barnard's Star's brightness, noting only one possible starspot over 130 days.
Stellar activity of this sort has created interest in using Barnard's Star as a proxy to understand similar stars. Photometric studies of its X-ray and UV emissions are hoped to shed light on the large population of old M dwarfs in the galaxy. Such research has astrobiological implications: given that the habitable zones of M dwarfs are close to the star, any planets would be strongly influenced by solar flares, winds, and plasma ejection events.
The star's neighborhood
Barnard's Star shares much the same neighborhood as the Sun. The neighbors of Barnard's Star are generally of red dwarf size, the smallest and most common star type. Its closest neighbor is currently the red dwarf Ross 154, at 1.66 parsecs or 5.41 light years distance. The Sun and Alpha Centauri are, respectively, the next closest systems. From Barnard's Star, the Sun would appear on the diametrically opposite side of the sky at coordinates RA=5h 57m 48.5s, Dec=−04° 41′ 36″, in the eastern part of the constellation Monoceros. The absolute magnitude of the Sun is 4.83 and at a distance of 1.834 parsecs, it would be an impressively bright first-magnitude star, as Pollux is from the Earth.
Notes and references
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- This parallax measurement and the subsequent distance calculation are taken from Benedict et al. (1999). SIMBAD suggests less precise parallax by van Leeuwen (2007) of 548.31 ± 1.51 mas and thus a slightly lesser distance from the Sun of 5.95 ly (1.82 pc).
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- The Sun's apparent magnitude from Barnard's Star, assuming negligible extinction: .
- Weighted parallax based on parallaxes from van Altena et al. (1995), Benedict et al. (1999) and van Leeuwen (2007).
|Wikimedia Commons has media related to Barnard's Star.|
- "Barnard's Star". SolStation.
- Darling, David. "Barnard's Star". The Encyclopedia of Astrobiology, Astronomy, and Spaceflight.
- Schmidling, Jack. "Barnard's Star". Jack Schmidling Productions, Inc. Amateur work showing Barnard's Star movement over time.
- Johnson, Rick. "Barnard's Star". Animated image with frames approx. one year apart, beginning in 2007, showing the movement of Barnard's Star.