Stellar kinematics

In astronomy, stellar kinematics is the observational study or measurement of the kinematics or motions of stars through space. The subject of stellar kinematics encompasses the measurement of stellar velocities in the Milky Way and its satellites as well as the measurement of the internal kinematics of more distant galaxies. Measurement of the kinematics of stars in different subcomponents of the Milky Way including the thin disk, the thick disk, the bulge, and the stellar halo provides important information about the formation and evolutionary history of our Galaxy. Kinematic measurements can also identify exotic phenomena such as hypervelocity stars escaping from the Milky Way, which are interpreted as the result of gravitational encounters of binary stars with the supermassive black hole at the Galactic Center.

Stellar kinematics is related to but distinct from the subject of stellar dynamics, which involves the theoretical study or modeling of the motions of stars under the influence of gravity. Stellar-dynamical models of systems such as galaxies or star clusters are often compared with or tested against stellar-kinematic data to study their evolutionary history and mass distributions, and to detect the presence of dark matter or supermassive black holes through their gravitational influence on stellar orbits.

Space velocity

Relation between proper motion and velocity components of an object. At emission, the object was at distance d from the Sun, and moved at angular rate μ radian/s, that is, μ = vt / d with vt = the component of velocity transverse to line of sight from the Sun. (The diagram illustrates an angle μ swept out in unit time at tangential velocity vt.)

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[4]

(U, V, W) = (11.1, 12.24, 7.25) km/s,

with statistical uncertainty (+0.69−0.75, +0.47−0.47, +0.37−0.36) km/s and systematic uncertainty (1, 2, 0.5) km/s. (Note that V is 7 km/s larger than estimated in 1999 by Dehnen et al.[5])

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 Milky Way.[6] 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.[7]

Within the Milky Way, 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 Milky Way, forming a strong correlation between the motion and chemical composition, thus indicating different formation mechanisms. The halo may be further subdivided into an inner and outer halo, with the inner halo having a net prograde motion with respect to the Milky Way and the outer a net retrograde motion.[8]

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 that 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, of which the star was formerly a member, before it was hurled out.

Two possible mechanisms may give rise to a runaway star:

Although both mechanisms are possible, astronomers generally favour the supernova mechanism as more common 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 Milky Way 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 center of the Milky Way. Rather, they travel in elliptical orbits, which often take them well outside the plane of the Milky Way. Although their orbital velocities in the Milky Way 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 Milky Way 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 (designated as HVS or HV in stellar catalogues) are stars with velocities that are substantially different from that expected for a star belonging to the normal distribution of stars in a galaxy. Such stars may have velocities so great that they exceed the escape velocity of the galaxy.[11] Ordinary stars in the Milky Way have velocities on the order of 100 km/s, whereas hypervelocity stars (especially those near the center of the Milky Way, 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 Jack G. Hills in 1988,[12] and their existence confirmed by Warren Brown, Margaret Geller, Scott Kenyon, and Michael Kurtz in 2005.[13] As of 2008, 10 unbound HVSs were known, one of which was believed to have originated from the Large Magellanic Cloud rather than the Milky Way.[14] Further measurements placed its origin within the Milky Way.[15] Due to uncertainty about the mass distribution within the Milky Way, determining whether a HVS is unbound is difficult; five additional known high-velocity stars may be unbound from the Milky Way and 16 HVSs are thought to be bound. The nearest currently known HVS (HVS2) is about 19 kpc from the Sun.

It is believed that about 1000 HVSs exist in the Milky Way.[16] Considering that there are around 100 billion stars in the Milky Way, this is a minuscule fraction (~0.000001%).

Origin of hypervelocity stars

HVSs are believed to originate by close encounters of binary stars with the supermassive black hole in the center of the Milky Way. One of the two partners is captured by the black hole, whereas the other escapes with high velocity. Also, "captured" does not necessarily mean "swallowed", as the companion to the HVS may enter an orbit around the black hole. However, this can only happen if the binary stars are falling nearly directly toward the black hole from extremely far, otherwise the speed gain would not be sufficiently high.

Supernova-induced HVSs may also be possible, although they are presumably rare. In this scenario, a HVS is ejected from a close binary system as a result of the companion star undergoing a supernova explosion. Ejection velocities up to 770 km/s, as measured from the Galactic rest frame, are possible for late-type B-stars .[17] This mechanism can explain the origin of HVSs which are ejected from the Galactic disk.

Known HVSs are main-sequence stars with masses a few times that of the Sun. HVSs with smaller masses are also expected and G/K-dwarf HVS candidates have been found.

It has been suggested that the HVSs in the Milky Way are a result of the passage of an orbiting dwarf galaxy near the Milky Way. When the dwarf galaxy made its closest approach to the center of the Milky Way, it underwent intense gravitational tugs. These tugs boosted the energy of some of its stars so much that they broke free of the dwarf galaxy entirely and were thrown into space, due to the slingshot-like effect of the boost.[18]

Some neutron stars are inferred to be traveling with similar speeds. This could be related to 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 or the loss of their near partner during the supernova explosions that forms them. The neutron star RX J0822-4300, 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 the first way.[19]

Some kind of supernovas are expected to happen if a white dwarf collides with its nearby partner and consumes the outer matter of this partner. The white dwarf and its nearby partner have very high orbital velocities at this time. The huge mass lost of the white dwarf during the supernova causes the nearby partner to leave at its previous huge orbital speed of several hundred kilometers per second as a hypervelocity star. The supernova remnant of the exploding white dwarf leaves because of its own high orbital speed as a new fast traveling neutron star. This seems to be the most likely origin of most HVSs and fast traveling neutron stars.

Partial list of HVSs

As of 2014, 20 HVS were known.[20][21]

Kinematic groups

A set of stars with similar space motion and ages is known as a kinematic group.[22] 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.[23] 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.[24]

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.[25] 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.

Types

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.[25] A third category, R, was later suggested by Sidney van den Bergh for associations that illuminate reflection nebulae.[26] 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.[27] Some groups also display properties of both OB and T associations, so the categorization is not always clear-cut.

OB associations

Carina OB1, a large OB association.

Young associations will contain 10–100 massive stars of spectral class O and B, and are known as OB associations. In addition, these associations also contain hundreds or thousands of low- and intermediate-mass stars. Association members 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.[28] It is believed that the majority of all stars in the Milky Way were formed in OB associations.[28] 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.[29] The nearest OB association is the Scorpius-Centaurus Association, located about 400 light years from the Sun.[30]

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.[31]

T associations

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.[32] 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. Group members have the same age and origin, the same chemical composition, and the same amplitude and direction in their vector of velocity.

R associations

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.[26] These young stellar groupings contain main sequence stars that are not sufficiently massive to disperse the interstellar clouds in which they formed.[27] 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.[33] An example of an R association is Monoceros R2, located 830 ± 50 parsecs from the Sun.[27]

Moving groups

If the remnants of a stellar association drift through the Milky Way as a somewhat coherent assemblage, then they are termed a moving group or kinematic group. Moving groups can be old, such as the HR 1614 moving group at 2 billion years, or young, such as the AB Dor Moving Group at only 120 million years.

Moving groups were studied intensely by Olin Eggen in the 1960s.[34] A list of the nearest young moving groups has been compiled by López-Santiago et al.[35] 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, although 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 nearby kinematic groups include:[36]

See also

References

  1. ↑ "Stellar Motions (Extension)". Australia Telescope Outreach and Education. Commonwealth Scientific and Industrial Research Organisation. 2005-08-18. Retrieved 2008-11-19.
  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. ↑ Schönrich, Ralph; Binney, James (2010). "Local kinematics and the local standard of rest". Monthly Notices of the Royal Astronomical Society. 403 (4): 1829–1833. Bibcode:2010MNRAS.403.1829S. arXiv:0912.3693 Freely accessible. doi:10.1111/j.1365-2966.2010.16253.x.
  5. ↑ Dehnen, Walter; Binney, James J. (1999). "Local stellar kinematics from HIPPARCOS data". Monthly Notices of the Royal Astronomical Society. 298 (2): 387–394. Bibcode:1998MNRAS.298..387D. arXiv:astro-ph/9710077 Freely accessible. doi:10.1046/j.1365-8711.1998.01600.x.
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  7. ↑ 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.
  8. ↑ 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. PMID 18075581. arXiv:0706.3005 Freely accessible. doi:10.1038/nature06460.
  9. ↑ Blaauw (1961), "On the origin of the O- and B-type stars with high velocities (the run-away stars), and some related problems" BAN 15, 265
  10. ↑ Tauris & Takens (1998), "Runaway velocities of stellar components originating from disrupted binaries via asymmetric supernova explosions" A&A 330, 1047
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  22. ↑ 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. Bibcode:2006ApJ...643.1160L. arXiv:astro-ph/0601573 Freely accessible. doi:10.1086/503183.
  23. ↑ 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. Bibcode:2001MNRAS.328...45M. arXiv:astro-ph/0106537 Freely accessible. doi:10.1046/j.1365-8711.2001.04781.x.
  24. ↑ Johnston, Kathryn V. (1995). "Fossil Signatures of Ancient Accretion Events in the Halo". The Astrophysical Journal. 465: 278. Bibcode:1996ApJ...465..278J. arXiv:astro-ph/9602060 Freely accessible. doi:10.1086/177418.
  25. 1 2 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.
  26. 1 2 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.
  27. 1 2 3 Herbst, W.; Racine, R. (1976). "R associations. V. MON R2". Astronomical Journal. 81: 840. Bibcode:1976AJ.....81..840H. doi:10.1086/111963.
  28. 1 2 "OB Associations" (PDF). GAIA: Composition, Formation and Evolution of the Galaxy. 2000-04-06. Retrieved 2013-11-14.
  29. ↑ de Zeeuw, P. T.; Hoogerwerf, R.; de Bruijne, J. H. J.; Brown, A. G. A.; et al. (1999). "A HIPPARCOS Census of the Nearby OB Associations". The Astronomical Journal. 117 (1): 354–399. Bibcode:1999AJ....117..354D. arXiv:astro-ph/9809227 Freely accessible. doi:10.1086/300682.
  30. ↑ Maíz-Apellániz, Jesús (2001). "The Origin of the Local Bubble". The Astrophysical Journal. 560 (1): L83–L86. Bibcode:2001ApJ...560L..83M. arXiv:astro-ph/0108472 Freely accessible. doi:10.1086/324016.
  31. ↑ 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.
  32. ↑ 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. Bibcode:1997A&A...325..613F. arXiv:astro-ph/9704281 Freely accessible.
  33. ↑ Herbst, W. (1975). "R-associations III. Local optical spiral structure". Astronomical Journal. 80: 503. Bibcode:1975AJ.....80..503H. doi:10.1086/111771.
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  36. ↑ 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. Bibcode:2006ApJ...643.1160L. arXiv:astro-ph/0601573 Freely accessible. doi:10.1086/503183.
  37. 1 2 3 Song, Inseok; et al. (December 2003), "New Members of the TW Hydrae Association, β Pictoris Moving Group, and Tucana/Horologium Association", The Astrophysical Journal, 599 (1): 342−350, Bibcode:2003ApJ...599..342S, doi:10.1086/379194.
  38. ↑ Wylie-de Boer, Elizabeth; et al. (February 2010), "Evidence of Tidal Debris from ω Cen in the Kapteyn Group", The Astronomical Journal, 139 (2): 636−645, Bibcode:2010AJ....139..636W, doi:10.1088/0004-6256/139/2/636.
  39. ↑ McDonald, A. R. E.; Hearnshaw, J. B. (August 1983), "The Wolf 630 moving group of stars", Monthly Notices of the Royal Astronomical Society, 204: 841−852, Bibcode:1983MNRAS.204..841M, doi:10.1093/mnras/204.3.841.

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