Fundamental relations for the velocity dispersion of stars in the Milky Way

被引：57

作者：

Sharma, Sanjib ^{[1
,2
]}

Hayden, Michael R. ^{[1
,2
]}

Bland-Hawthorn, Joss ^{[1
,2
]}

Stello, Dennis ^{[2
,3
,4
]}

Buder, Sven ^{[2
,5
,6
]}

Zinn, Joel C. ^{[3
]}

Kallinger, Thomas ^{[7
]}

Asplund, Martin ^{[8
]}

De Silva, Gayandhi M. ^{[9
]}

D'Orazi, Valentina ^{[10
]}

Freeman, Ken ^{[6
]}

Kos, Janez ^{[11
]}

Lewis, Geraint F. ^{[1
]}

Lin, Jane ^{[6
]}

Lind, Karin ^{[12
]}

Martell, Sarah ^{[2
,3
]}

Simpson, Jeffrey D. ^{[3
]}

Wittenmyer, Rob A. ^{[13
]}

Zucker, Daniel B. ^{[9
,14
]}

Zwitter, Tomaz ^{[11
]}

Chen, Boquan ^{[1
]}

Cotar, Klemen ^{[11
]}

Esdaile, James ^{[3
]}

Hon, Marc ^{[3
]}

Horner, Jonathan ^{[13
]}

Huber, Daniel ^{[15
]}

Kafle, Prajwal R. ^{[16
]}

Khanna, Shourya ^{[1
]}

Ting, Yuan-Sen ^{[6
,17
,18
,19
]}

Nataf, David M. ^{[20
]}

Nordlander, Thomas ^{[2
,6
]}

Saadon, Mohd Hafiz Mohd ^{[3
,21
]}

Tepper-Garcia, Thor ^{[1
]}

Tinney, C. G. ^{[22
]}

Traven, Gregor ^{[23
]}

Watson, Fred ^{[24
]}

Wright, Duncan ^{[13
]}

Wyse, Rosemary F. G. ^{[20
]}

机构：

[1] Univ Sydney, Sch Phys, Sydney Inst Astron, A28, Sydney, NSW 2006, Australia

[2] ARC Ctr Excellence All Sky Astrophys Three Dimens, Weston, ACT 2611, Australia

[3] Univ New South Wales, Sch Phys, Sydney, NSW 2052, Australia

[4] Aarhus Univ, Stellar Astrophys Ctr, Dept Phys & Astron, DK-8000 Aarhus C, Denmark

[5] Max Planck Inst Astron MPIA, Koenigstuhl 17, D-69117 Heidelberg, Germany

[6] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia

[7] Univ Vienna, Inst Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria

[8] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany

[9] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia

[10] INAF Osservatorio Astron Padova, I-35122 Padua, Italy

[11] Univ Ljubljana, Fac Math & Phys, Jadranska 19, Ljubljana 1000, Slovenia

[12] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, SE-10691 Stockholm, Sweden

[13] Univ Southern Queensland, Ctr Astrophys, Toowoomba, Qld 4350, Australia

[14] Macquarie Univ, Res Ctr Astron Astrophys & Astrophoton, Sydney, NSW 2109, Australia

[15] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA

[16] Univ Western Australia, Int Ctr Radio Astron Res ICRAR, 35 Stirling Highway, Crawley, WA 6009, Australia

[17] Inst Adv Study, Princeton, NJ 08540 USA

[18] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA

[19] Observ Carnegie Inst Washington, 813 Santa Barbara St, Pasadena, CA 91101 USA

[20] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA

[21] Univ Malaya, Acad Islamic Studies, Dept Fiqh & Usul, Kuala Lumpur 50603, Malaysia

[22] Univ New South Wales, Sch Phys, Exoplanetary Sci UNSW, Sydney, NSW 2052, Australia

[23] Lund Observ, Dept Astron & Theoret Phys, Box 43, SE-22100 Lund, Sweden

[24] Dept Ind Innovat & Sci, 105 Delhi Rd, N Ryde, NSW 2113, Australia

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2021年 / 506卷 / 02期

基金：

澳大利亚研究理事会; 瑞典研究理事会; 美国国家航空航天局; 美国国家科学基金会;

关键词：

Galaxy: disc; Galaxy: evolution; Galaxy: formation; Galaxy: kinematics and dynamics; SPIRAL GALAXIES; GALAH SURVEY; SOLAR NEIGHBORHOOD; RADIAL MIGRATION; GALACTIC DISC; DYNAMICAL EVOLUTION; ASTEROSEISMIC MASS; ANGULAR-MOMENTUM; AGE; METALLICITY;

D O I：

10.1093/mnras/stab1086

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We explore the fundamental relations governing the radial and vertical velocity dispersions of stars in the Milky Way, from combined studies of complementary surveys including GALAH, LAMOST, APOGEE, the NASA Kepler and K2 missions, and Gaia DR2. We find that different stellar samples, even though they target different tracer populations and employ a variety of age estimation techniques, follow the same set of fundamental relations. We provide the clearest evidence to date that, in addition to the well-known dependence on stellar age, the velocity dispersions of stars depend on orbital angular momentum L-z, metallicity, and height above the plane vertical bar z vertical bar, and are well described by a multiplicatively separable functional form. The dispersions have a power-law dependence on age with exponents of 0.441 +/- 0.007 and 0.251 +/- 0.006 for sigma(z) and sigma(R), respectively, and the power law is valid even for the oldest stars. For the solar neighbourhood stars, the apparent break in the power law for older stars, as seen in previous studies, is due to the anticorrelation of L-z with age. The dispersions decrease with increasing L-z until we reach the Sun's orbital angular momentum, after which sigma(z) increases (implying flaring in the outer disc) while sigma(R) flattens. For a given age, the dispersions increase with decreasing metallicity, suggesting that the dispersions increase with birth radius. The dispersions also increase linearly with vertical bar z vertical bar. The same set of relations that work in the solar neighbourhood also work for stars between 3 < R/kpc < 20. Finally, the high-[alpha/Fe] stars follow the same relations as the low-[alpha/Fe] stars.

引用

页码：1761 / 1776

页数：16

共 97 条

[1] Confirming chemical clocks: asteroseismic age dissection of the Milky Way disc(s) [J].