The Gaia-ESO Survey: A lithium-rotation connection at 5 Myr?

被引：44

作者：

Bouvier, J. ^{[1
,2
]}

Lanzafame, A. C. ^{[3
,4
]}

Venuti, L. ^{[1
,2
,5
]}

Klutsch, A. ^{[4
]}

Jeffries, R. ^{[6
]}

Frasca, A. ^{[4
]}

Moraux, E. ^{[1
,2
]}

Biazzo, K. ^{[4
]}

Messina, S. ^{[4
]}

Micela, G. ^{[5
]}

Randich, S. ^{[7
]}

Stauffer, J. ^{[8
]}

Cody, A. M. ^{[9
]}

Flaccomio, E. ^{[5
,7
]}

Gilmore, G. ^{[10
]}

Bayo, A. ^{[11
]}

Bensby, T. ^{[12
]}

Bragaglia, A. ^{[13
]}

Carraro, G. ^{[14
]}

Casey, A. ^{[10
]}

Costado, M. T. ^{[15
]}

Damiani, F. ^{[5
]}

Delgado Mena, E. ^{[16
]}

Donati, P. ^{[13
]}

Franciosini, E.

Hourihane, A. ^{[10
]}

Koposov, S. ^{[10
]}

Lardo, C. ^{[17
]}

Lewis, J. ^{[10
]}

Magrini, L. ^{[7
]}

Monaco, L. ^{[18
]}

Morbidelli, L. ^{[7
]}

Prisinzano, L. ^{[5
]}

Sacco, G. ^{[7
]}

Sbordone, L. ^{[19
]}

Sousa, S. G. ^{[16
]}

Vallenari, A.

Worley, C. C. ^{[10
]}

Zaggia, S. ^{[20
]}

Zwitter, T. ^{[21
]}

机构：

[1] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France

[2] CNRS, IPAG, F-38000 Grenoble, France

[3] Univ Catania, Dipartimento Fis & Astron, Sez Astrofis, Via S Sofia 78, I-95123 Catania, Italy

[4] INAF Osservatorio Astrofis Catania, Via S Sofia 78, I-95123 Catania, Italy

[5] INAF Osservatorio Astron Palermo GS Vaiana, Piazza Parlamento 1, I-90134 Palermo, Italy

[6] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England

[7] INAF Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy

[8] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA

[9] NASA, Ames Res Ctr, Kepler Sci Off, Moffett Field, CA 94035 USA

[10] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England

[11] Univ Valparaiso, Inst Fis & Astron, Valparaiso, Chile

[12] Lund Observ, Dept Astron & Theoret Phys, Box 43, S-22100 Lund, Sweden

[13] INAF Osservatorio Astron Bologna, Via Ranzani 1, I-40127 Bologna, Italy

[14] European So Observ, Alonso de Cordova 3107, Santiago, Chile

[15] CSIC, Inst Astrofis Andalucia, Apdo 3004, E-18008 Granada, Spain

[16] Univ Porto, Inst Astrofis & Ciencias Espaco, CAUP, Rua Estrelas, P-4150762 Porto, Portugal

[17] Liverpool John Moores Univ, Astrophys Res Inst, 146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England

[18] Univ Andres Bello, Fac Ciencias Exactas, Dept Ciencias Fis, Fernandez Concha 700, Santiago, Chile

[19] Pontificia Univ Catolica Chile, Millennium Inst Astrophys, Vicuna Mackenna 4860, Santiago, Chile

[20] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy

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

来源：

ASTRONOMY & ASTROPHYSICS | 2016年 / 590卷

基金：

英国科学技术设施理事会;

关键词：

stars: abundances; stars: pre-main sequence; stars: rotation; open clusters and associations: individual: NGC 2264; PRE-MAIN-SEQUENCE; LOW-MASS STARS; SOLAR-TYPE STARS; NGC; 2264; EVOLUTIONARY MODELS; MAGNETIC-FIELDS; PMS STARS; ABUNDANCES; ACCRETION; YOUNG;

D O I：

10.1051/0004-6361/201628336

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. The evolution of lithium abundance in cool dwarfs provides a unique probe of nonstandard processes in stellar evolution. Aims. We investigate the lithium content of young low-mass stars in the 5 Myr old, star forming region NGC 2264 and its relationship with rotation. Methods. We combine lithium equivalent width measurements (EW(Li)) from the Gaia-ESO Survey with the determination of rotational periods from the CSI 2264 survey. We only consider bona fide nonaccreting cluster members to minimize the uncertainties on EW(Li). Results. We report the existence of a relationship between lithium content and rotation in NGC 2264 at an age of 5 Myr. The Li-rotation connection is seen over a restricted temperature range (T-eff = 3800-4400 K), where fast rotators are Li-rich compared to slow rotators. This correlation is similar to, albeit of lower amplitude than, the Li-rotation connection previously reported for K dwarfs in the 125 Myr old Pleiades cluster. We investigate whether the nonstandard pre-main-sequence models developed so far to explain the Pleiades results, which are based on episodic accretion, pre-main-sequence, core-envelope decoupling, and/or radius inflation due to enhanced magnetic activity, can account for early development of the Li-rotation connection. While radius inflation appears to be the most promising possibility, each of these models has issues. We therefore also discuss external causes that might operate during the first few Myr of pre-main-sequence evolution, such as planet engulfment and/or steady disk accretion, as possible candidates for the common origin for Li excess and fast rotation in young low-mass pre-main-sequence stars. Conclusions. The emergence of a connection between lithium content and rotation rate at such an early age as 5 Myr suggests a complex link between accretion processes, early angular momentum evolution, and possibly planet formation, which likely impacts early stellar evolution and has yet to be fully deciphered.

引用

页数：9

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