Stellar kinematics

Stellar kinematics

Stellar kinematics is the study of the movement of stars without needing to understand how they acquired their motion. This differs from stellar dynamics, which takes into account gravitational effects. The motion of a star relative to the Sun can provide useful information about the origin and age of a star, as well as the structure and evolution of the surrounding galaxy.

In astronomy, it is widely accepted that most stars are born within molecular clouds known as stellar nurseries. The stars formed within such a cloud compose open clusters containing dozens to thousands of members. These clusters dissociate with time. Stars that separate themselves from the cluster's core are designated as members of the cluster's stellar association. If the remnant later drifts through the galaxy as a somewhat coherent assemblage, then it is termed a moving group.


Space velocity

The component of stellar motion toward or away from the Sun, known as radial velocity, can be measured from the spectrum shift caused by the Doppler effect. The transverse, or proper motion must be found by taking a series of positional determinations against more distant objects. Once the distance to a star is determined through astrometric means such as parallax, the space velocity can be computed.[1] This is the star's actual motion relative to the Sun or the local standard of rest (LSR). The latter is typically taken as a position at the Sun's present location that is following a circular orbit around the galactic center at the mean velocity of those nearby stars with low velocity dispersion.[2] The Sun's motion with respect to the LSR is called the peculiar solar motion.

The components of space velocity in the Milky Way's Galactic coordinate system are usually designated U, V, and W, given in km/s, with U positive in the direction of the Galactic center, V positive in the direction of galactic rotation, and W positive in the direction of the North Galactic Pole.[3] The peculiar motion of the Sun with respect to the LSR is (U, V, W) = (10.00 ± 0.36, 5.23 ± 0.62, 7.17 ± 0.38) km/s.[4]

The stars in the Milky Way can be subdivided into two general populations, based on their metallicity, or proportion of elements with atomic numbers higher than helium. Among nearby stars, it has been found that population I, higher metallicity stars have generally lower velocities than older, population II stars. The latter have elliptical orbits that are inclined to the plane of the galaxy.[5] Comparison of the kinematics of nearby stars has also led to the identification of stellar associations. These are most likely groups of stars that share a common point of origin in giant molecular clouds.[6]

Within the Milky Way galaxy, there are three primary components of stellar kinematics: the disk, halo and bulge or bar. These kinematic groups are closely related to the stellar populations in the galaxy, forming a strong correlation between the motion and chemical composition, thus indicating different formation mechanisms. The halo may be further sub-divided into an inner and outer halo, with the inner halo having a net prograde rotation with respect to the galaxy and the outer a net retrograde movement.[7]

High-velocity stars

Depending on the definition, a high-velocity star is a star moving faster than 65 km/s to 100 km/s relative to the average motion of the stars in the Sun's neighbourhood. The velocity is also sometimes defined as supersonic relative to the surrounding interstellar medium. The three types of high-velocity stars are: runaway stars, halo stars and hypervelocity stars.

Runaway stars

Four runaway stars plowing through regions of dense interstellar gas and creating bright bow waves and trailing tails of glowing gas. The stars in these NASA Hubble Space Telescope images are among 14 young runaway stars spotted by the Advanced Camera for Surveys between October 2005 and July 2006

A runaway star is one which is moving through space with an abnormally high velocity relative to the surrounding interstellar medium. The proper motion of a runaway star often points exactly away from a stellar association, whose member it therefore once must have been before it was hurled out.

Two possible mechanisms may give rise to a runaway star:

  • In the first scenario, a close encounter between two binary systems may result in the disruption of both systems, with some of the stars being ejected at high velocities.
  • In the second scenario, a supernova explosion in a multiple star system can result in the remaining components moving away at high speed.

While both mechanisms are theoretically possible, astronomers generally favour the supernova hypothesis as more likely in practice.

One example of a related set of runaway stars is the case of AE Aurigae, 53 Arietis and Mu Columbae, all of which are moving away from each other at velocities of over 100 km/s (for comparison, the Sun moves through the galaxy at about 20 km/s faster than the local average). Tracing their motions back, their paths intersect near to the Orion Nebula about 2 million years ago. Barnard's Loop is believed to be the remnant of the supernova that launched the other stars.

Another example is the X-ray object Vela X-1, where photodigital techniques reveal the presence of a typical supersonic bow shock hyperbola.

Halo stars

High-velocity stars are very old stars that do not share the motion of the Sun or most other stars in the solar neighbourhood which are in similar circular orbits around the centre of the Galaxy. Rather, they travel in elliptical orbits, which often take them well outside the plane of the Galaxy. Although their orbital velocities in the Galaxy may be no faster than the Sun’s, their different paths result in the high relative velocities.

Typical examples are the halo stars passing through the disk of the galaxy at steep angles. One of the nearest 45 stars, called Kapteyn's star, is an example of the high-velocity stars that lie near the Sun. Its observed radial velocity is -245 km/s, and the components of its space velocity are U = 19 km/s, V = -288 km/s, and W = -52 km/s.

Hypervelocity stars

Hypervelocity stars (HVSs), or, less formally, Exiled Stars,[8] are stars with a velocity so great that they are able to escape the gravitational pull of the galaxy. Ordinary stars in the galaxy have velocities on the order of 100 km/s, while hypervelocity stars (especially those near the center of the galaxy, which is where most are thought to be "produced"), have velocities on the order of 1000 km/s.

The existence of HVSs was first predicted by J. Hills in 1988.[9] The first HVS was discovered in 2005 by Warren Brown and collaborators[10] at the Harvard-Smithsonian Center for Astrophysics. Currently, sixteen are known, one of which is believed to originate from the Large Magellanic Cloud rather than the Milky Way.[11] All of the currently known HVSs are over 50,000 parsecs away and are unbound from the galaxy.

It is believed that about 1000 HVSs exist in our Galaxy. Considering that there are around 100 billion stars in the Milky Way, this is a minuscule fraction (~0.000001%).[citation needed]

Production methods

The main production method for HVSs is summarized as thus: they are believed to originate by close encounters of binary stars with the supermassive black hole in the centre of the Milky Way. One of the two partners is captured by the black hole, while the other escapes with high velocity. Also, it is worth noting that "captured" does not necessarily mean "swallowed", for in all likelihood the companion to the HVS will never fall into the black hole.

Known HVSs are main-sequence stars with masses a few times that of the Sun.

A team at Argentina's Cordoba Observatory believe that our HVS are a result of a merging with a collision between the Milky Way, and an orbiting dwarf galaxy. A dwarf galaxy that has been orbiting the Milky Way, passed through the centre of the Milky Way. When the dwarf galaxy made its closest approach to the centre of the Milky Way, it underwent intense gravitational tugs. These tugs boosted the energy of some its stars so much that they broke free of the dwarf galaxy entirely and were thrown into space.[12]

Some neutron stars are inferred to be traveling with similar speeds, however they are unrelated to both HVSs and the HVS ejection mechanism. Neutron stars are the remnants of supernova explosions, and their extreme speeds are very likely the result of an asymmetric supernova explosion. The neutron star RX J0822-4300,[13] which was measured to move at a record speed of over 1500 km/s (0.5% c) in 2007 by the Chandra X-ray Observatory, is thought to have been produced this way.

List of HVSs

  • HVS 1 - (SDSS J090744.99+024506.8) (a.k.a. The Outcast Star) - the first hypervelocity star to be discovered[10]
  • HVS 2 - (SDSS J093320.86+441705.4) or (US 708)
  • HVS 3 - (HE 0437-5439) - possibly from the Large Magellanic Cloud[11]
  • HVS 4 - (SDSS J091301.00+305120.0)
  • HVS 5 - (SDSS J091759.42+672238.7)
  • HVS 6 - (SDSS J110557.45+093439.5)
  • HVS 7 - (SDSS J113312.12+010824.9)
  • HVS 8 - (SDSS J094214.04+200322.1)
  • HVS 9 - (SDSS J102137.08-005234.8)
  • HVS 10 - (SDSS J120337.85+180250.4)

Kinematic groups

A set of stars with similar space motion and ages is known as a kinematic group.[14] These are stars that could share a common origin, such as the evaporation of an open cluster, the remains of a star forming region, or collections of overlapping star formation bursts at differing time periods in adjacent regions.[15] Most stars are born within molecular clouds known as stellar nurseries. The stars formed within such a cloud compose gravitationally bound open clusters containing dozens to thousands of members with similar ages and compositions. These clusters dissociate with time. Groups of young stars that escape a cluster, or are no longer bound to each other, form stellar associations. As these stars age and disperse, their association is no longer readily apparent and they become moving groups of stars.

Astronomers are able to determine if stars are members of a kinematic group because they share the same age, metallicity, and kinematics (radial velocity and proper motion). As the stars in a moving group formed in proximity and at nearly the same time from the same gas cloud, although later disrupted by tidal forces, they share similar characteristics.[16]

Stellar associations

A stellar association is a very loose star cluster, whose stars share a common origin, but have become gravitationally unbound and are still moving together through space. Associations are primarily identified by their common movement vectors and ages. Identification by chemical composition is also used to factor in association memberships.

Stellar associations were first discovered by the Armenian astronomer Viktor Ambartsumian in 1947.[17] The conventional name for an association uses the names or abbreviations of the constellation (or constellations) in which they are located; the association type, and, sometimes, a numerical identifier.


Infrared ESO's VISTA view of a stellar nursery in Monoceros.

Viktor Ambartsumian first categorized stellar associations into two groups, OB and T, based on the properties of their stars.[17] A third category, R, was later suggested by Sidney van den Bergh for associations that illuminate reflection nebulae.[18] The OB, T, and R associations form a continuum of young stellar groupings. But it is currently uncertain whether they are an evolutionary sequence, or represent some other factor at work.[19] Some groups also display properties of both OB and T associations, so the categorization is not always clear-cut.

Young associations will contain 10–100 massive stars of spectral class O and B, and are known as OB associations. These are believed to form within the same small volume inside a giant molecular cloud. Once the surrounding dust and gas is blown away, the remaining stars become unbound and begin to drift apart.[20] It is believed that the majority of all stars in the Milky Way were formed in OB associations.[20] O class stars are short-lived, and will expire as supernovae after roughly a million years. As a result, OB associations are generally only a few million years in age or less. The O-B stars in the association will have burned all their fuel within 10 million years. (Compare this to the current age of the Sun at about 5 billion years.)

The Hipparcos satellite provided measurements that located a dozen OB associations within 650 parsecs of the Sun.[21] The nearest OB association is the Scorpius-Centaurus Association, located about 400 light years from the Sun.[22]

OB associations have also been found in the Large Magellanic Cloud and the Andromeda Galaxy. These associations can be quite sparse, spanning 1,500 light years in diameter.[23]

Young stellar groups can contain a number of infant T Tauri stars that are still in the process of entering the main sequence. These sparse populations of up to a thousand T Tauri stars are known as T associations. The nearest example is the Taurus-Auriga T association (Tau-Aur T association), located at a distance of 140 parsecs from the Sun.[24] Other examples of T associations include the R Corona Australis T association, the Lupus T association, the Chamaeleon T association and the Velorum T association. T associations are often found in the vicinity of the molecular cloud from which they formed. Some, but not all, include O-B class stars. To summarize the characteristics of Moving groups members: they have the same age and origin, the same chemical composition and they have the same amplitude and direction in their vector of velocity.

Associations of stars that illuminate reflection nebulae are called R associations, a name suggested by Sidney van den Bergh after he discovered that the stars in these nebulae had a non-uniform distribution.[18] These young stellar groupings contain main sequence stars that are not sufficiently massive to disperse the interstellar clouds in which they formed.[19] This allows the properties of the surrounding dark cloud to be examined by astronomers. Because R-associations are more plentiful than OB associations, they can be used to trace out the structure of the galactic spiral arms.[25] An example of an R-association is Monoceros R2, located 830 ± 50 parsecs from the Sun.[19]

Moving groups

If the remnants of a stellar association drift through the galaxy as a somewhat coherent assemblage, then they are termed a moving group. Moving groups can be old, such as the HR 1614 moving group at 2 billion years, or young, such as the AB Doradus moving group at only 50 million.

Moving groups were studied intensely by Olin Eggen in the 1960s[26] A list of the nearest young moving groups has been compiled by López-Santiago et al.[27] The closest is the Ursa Major Moving Group which includes all of the stars in the Plough/Big Dipper asterism except for α Ursae Majoris and η Ursae Majoris. This is sufficiently close that the Sun lies in its outer fringes, without being part of the group. Hence, while members are concentrated at declinations near 60° N, some outliers are as far away across the sky as Triangulum Australe at 70° S.

Stellar streams

A stellar stream is an association of stars orbiting a galaxy that was once a globular cluster or dwarf galaxy that has now been torn apart and stretched out along its orbit by tidal forces.

Known kinematic groups

Some kinematic groups include:[28]

See also


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  2. ^ Fich, Michel; Tremaine, Scott (1991). "The mass of the Galaxy". Annual review of astronomy and astrophysics 29 (1): 409–445. Bibcode 1991ARA&A..29..409F. doi:10.1146/annurev.aa.29.090191.002205. 
  3. ^ Johnson, Dean R. H.; Soderblom, David R. (1987). "Calculating galactic space velocities and their uncertainties, with an application to the Ursa Major group". Astronomical Journal 93 (2): 864–867. Bibcode 1987AJ.....93..864J. doi:10.1086/114370. 
  4. ^ Dehnen, Walter; Binney, James J. (1999). "Local stellar kinematics from HIPPARCOS data". Monthly Notices of the Royal Astronomical Society 298 (2): 387–394. arXiv:astro-ph/9710077. Bibcode 1998MNRAS.298..387D. doi:10.1046/j.1365-8711.1998.01600.x. 
  5. ^ Johnson, Hugh M. (1957). "The Kinematics and Evolution of Population I Stars". Publications of the Astronomical Society of the Pacific 69 (406): 54. Bibcode 1957PASP...69...54J. doi:10.1086/127012. 
  6. ^ Elmegreen, B.; Efremov, Y. N. (1999). "The Formation of Star Clusters". American Scientist 86 (3): 264. Bibcode 1998AmSci..86..264E. doi:10.1511/1998.3.264. 
  7. ^ Carollo, Daniela et al. (2007-12-13). "Two stellar components in the halo of the Milky Way". Nature 450 (7172): 1020–1025. Bibcode 2007Natur.450.1020C. doi:10.1038/nature06460. PMID 18075581. 
  8. ^ "Two Exiled Stars Are Leaving Our Galaxy Forever". Space Daily. 2006-01-27. Retrieved 2009-09-24. 
  9. ^ Hills, J. G. (1988). "Hyper-velocity and tidal stars from binaries disrupted by a massive Galactic black hole". Nature 331 (6158): 687–689. Bibcode 1988Natur.331..687H. doi:10.1038/331687a0. 
  10. ^ a b Brown, Warren R.; Geller, Margaret J.; Kenyon, Scott J.; Kurtz, Michael J. (2005). "Discovery of an Unbound Hypervelocity Star in the Milky Way Halo". Astrophysical Journal 622 (1): L33–L36. arXiv:astro-ph/0501177. Bibcode 2005ApJ...622L..33B. doi:10.1086/429378. 
  11. ^ a b Edelmann, H.; Napiwotzki, R.; Heber, U.; Christlieb, N.; Reimers, D. (2005). "HE 0437-5439: An Unbound Hypervelocity Main-Sequence B-Type Star". Astrophysical Journal 634 (2): L181–L184. arXiv:astro-ph/0511321. Bibcode 2005ApJ...634L.181E. doi:10.1086/498940. 
  12. ^ Maggie McKee (4 October 2008). "Milky Way's fastest stars may be immigrants.". New Scientist. 
  13. ^ Watzke, Megan (28 November 2007). "Chandra discovers cosmic cannonball". Newswise. 
  14. ^ López-Santiago, J.; Montes, D.; Crespo-Chacón, I.; Fernández-Figueroa, M. J. (June 2006). "The Nearest Young Moving Groups". The Astrophysical Journal 643 (2): 1160–1165. arXiv:astro-ph/0601573. Bibcode 2006ApJ...643.1160L. doi:10.1086/503183. 
  15. ^ Montes, D.; et al. (November 2001). "Late-type members of young stellar kinematic groups - I. Single stars". Monthly Notices of the Royal Astronomical Society 328 (1): 45–63. arXiv:astro-ph/0106537. Bibcode 2001MNRAS.328...45M. doi:10.1046/j.1365-8711.2001.04781.x. 
  16. ^ Johnston, Kathryn V. (1995). "Fossil Signatures of Ancient Accretion Events in the Halo". Bulletin of the American Astronomical Society 27: 1370. arXiv:astro-ph/9602060. Bibcode 1996ApJ...465..278J. doi:10.1086/177418. 
  17. ^ a b Israelian, Garik (1997). "Obituary: Victor Amazaspovich Ambartsumian, 1912 [i.e. 1908] -1996". Bulletin of the American Astronomical Society 29 (4): 1466–1467. Bibcode 1997BAAS...29.1466I. 
  18. ^ a b Herbst, W. (1976). "R associations. I - UBV photometry and MK spectroscopy of stars in southern reflection nebulae". Astronomical Journal 80: 212–226. Bibcode 1975AJ.....80..212H. doi:10.1086/111734. 
  19. ^ a b c Herbst, W.; Racine, R. (1976). "R associations. V. MON R2.". Astronomical Journal 81: 840. Bibcode 1976AJ.....81..840H. doi:10.1086/111963. 
  20. ^ a b "OB Associations". The GAIA Study Report: Executive Summary and Science Section. 2000-04-06. Retrieved 2006-06-08. 
  21. ^ de Zeeuw, P. T.; Hoogerwerf, R.; de Bruijne, J. H. J.; Brown, A. G. A.; Blaauw, A. (1999). "A HIPPARCOS Census of the Nearby OB Associations". The Astronomical Journal 117 (1): 354–399. arXiv:astro-ph/9809227. Bibcode 1999AJ....117..354D. doi:10.1086/300682. 
  22. ^ Maíz-Apellániz, Jesús (2001). "The Origin of the Local Bubble". The Astrophysical Journal 560 (1): L83–L86. arXiv:astro-ph/0108472. Bibcode 2001ApJ...560L..83M. doi:10.1086/324016. 
  23. ^ Elmegreen, B.; Efremov, Y. N. (1999). "The Formation of Star Clusters". American Scientist 86 (3): 264. Bibcode 1998AmSci..86..264E. doi:10.1511/1998.3.264. Retrieved 2006-08-23. 
  24. ^ Frink, S.; Roeser, S.; Neuhaeuser, R.; Sterzik, M. K. (1999). "New proper motions of pre-main-sequence stars in Taurus-Auriga". Astronomy and Astrophysics 325: 613–622. 
  25. ^ Herbst, W. (1975). "R-associations III. Local optical spiral structure". Astronomical Journal 80: 503. Bibcode 1975AJ.....80..503H. doi:10.1086/111771. 
  26. ^ Eggen, O.J. Moving Groups of Stars. Galactic structure, ed. Adriaan Blaauw and Maarten Schmidt. University of Chicago Press, Chicago, p. 111 (1965). Bibcode1965gast.conf..111E
  27. ^ López-Santiago, J; Montes, D; Crespo-Chacón, I; Fernández-Figueroa, MJ (2006). "The Nearest Young Moving Groups". The Astrophysical Journal 643 (2): 1160–1165. arXiv:astro-ph/0601573. Bibcode 2006ApJ...643.1160L. doi:10.1086/503183. 
  28. ^ López-Santiago, J.; Montes, D.; Crespo-Chacón, I.; Fernández-Figueroa, M. J. (June 2006). "The Nearest Young Moving Groups". The Astrophysical Journal 643 (2): 1160–1165. arXiv:astro-ph/0601573. Bibcode 2006ApJ...643.1160L. doi:10.1086/503183. 

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