VERY LOW MASS STELLAR AND SUBSTELLAR COMPANIONS TO SOLAR-LIKE STARS FROM MARVELS. II. A SHORT-PERIOD COMPANION ORBITING AN F STAR WITH EVIDENCE OF A STELLAR TERTIARY AND SIGNIFICANT MUTUAL INCLINATION

被引：16

作者：

Fleming, Scott W. ^{[1
,2
,3
]}

Ge, Jian ^{[1
]}

Barnes, Rory ^{[4
]}

Beatty, Thomas G. ^{[5
]}

Crepp, Justin R. ^{[6
]}

De Lee, Nathan ^{[1
,7
]}

Esposito, Massimiliano ^{[8
,9
]}

Femenia, Bruno ^{[8
,9
]}

Ferreira, Leticia ^{[10
,11
]}

Gary, Bruce ^{[7
]}

Gaudi, B. Scott ^{[5
]}

Ghezzi, Luan ^{[11
,12
]}

Gonzalez Hernandez, Jonay I. ^{[8
,9
]}

Hebb, Leslie ^{[7
]}

Jiang, Peng ^{[1
]}

Lee, Brian ^{[1
]}

Nelson, Ben ^{[1
]}

Porto De Mello, Gustavo F. ^{[10
,11
]}

Shappee, Benjamin J. ^{[5
]}

Stassun, Keivan ^{[7
,13
]}

Thompson, Todd A. ^{[5
]}

Tofflemire, Benjamin M. ^{[4
,14
]}

Wisniewski, John P. ^{[4
]}

Wood-Vasey, W. Michael ^{[15
]}

Agol, Eric ^{[4
]}

Allende Prieto, Carlos ^{[8
,9
]}

Bizyaev, Dmitry ^{[16
]}

Brewington, Howard ^{[16
]}

Cargile, Phillip A. ^{[7
]}

Coban, Louis ^{[15
]}

Costello, Korena S. ^{[15
]}

da Costa, Luis N. ^{[11
,12
]}

Good, Melanie L. ^{[15
]}

Hua, Nelson ^{[15
]}

Kane, Stephen R. ^{[17
]}

Lander, Gary R. ^{[15
]}

Liu, Jian ^{[1
]}

Ma, Bo ^{[1
]}

Mahadevan, Suvrath ^{[2
,3
]}

Maia, Marcio A. G. ^{[11
,12
]}

Malanushenko, Elena ^{[16
]}

Malanushenko, Viktor ^{[16
]}

Muna, Demitri ^{[18
]}

Nguyen, Duy Cuong ^{[1
,19
]}

Oravetz, Daniel ^{[16
]}

Paegert, Martin ^{[7
]}

Pan, Kaike ^{[16
]}

Pepper, Joshua ^{[7
]}

Rebolo, Rafael ^{[8
,9
,20
]}

Roebuck, Eric J. ^{[15
]}

机构：

[1] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32610 USA

[2] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA

[3] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA

[4] Univ Washington, Dept Astron, Seattle, WA 98195 USA

[5] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA

[6] CALTECH, Dept Astron, Pasadena, CA 91125 USA

[7] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA

[8] Inst Astrofis Canarias, E-38205 Tenerife, Spain

[9] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain

[10] Univ Fed Rio de Janeiro, Observ Valongo, BR-20080090 Rio De Janeiro, RJ, Brazil

[11] LIneA, Lab Interinst Astron, Rio De Janeiro, RJ, Brazil

[12] Observ Nacl, BR-20921400 Rio De Janeiro, Brazil

[13] Fisk Univ, Dept Phys, Nashville, TN 37208 USA

[14] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA

[15] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA

[16] Apache Point Observ, Sunspot, NM 88349 USA

[17] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA

[18] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA

[19] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA

[20] CSIC, E-28006 San Cristobal la Laguna, Spain

[21] Univ Fed Rio Grande do Sul, Inst Fis, BR-91501970 Porto Alegre, RS, Brazil

[22] Indian Inst Astrophys, Bangalore 560034, Karnataka, India

来源：

ASTRONOMICAL JOURNAL | 2012年 / 144卷 / 03期

基金：

美国国家科学基金会; 美国国家航空航天局; 美国安德鲁·梅隆基金会;

关键词：

binaries: close; binaries: spectroscopic; stars: individual (TYC 2930-00872-1); CLOSE BINARY STARS; RADIAL-VELOCITY; MAIN-SEQUENCE; EVOLUTIONARY MODELS; TIDAL FRICTION; HOT JUPITERS; TRIPLE; PLANETS; SPECTROGRAPH; ROTATION;

D O I：

10.1088/0004-6256/144/3/72

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report the discovery via radial velocity (RV) measurements of a short-period (P = 2.430420 +/- 0.000006 days) companion to the F-type main-sequence star TYC 2930-00872-1. A long-term trend in the RV data also suggests the presence of a tertiary stellar companion with P > 2000 days. High-resolution spectroscopy of the host star yields T-eff = 6427 +/- 33 K, log g = 4.52 +/- 0.14, and [Fe/H] = -0.04 +/- 0.05. These parameters, combined with the broadband spectral energy distribution (SED) and a parallax, allow us to infer a mass and radius of the host star of M-1 = 1.21 +/- 0.08 M-circle dot and R-1 = 1.09(-0.13)(+0.15) R-circle dot. The minimum mass of the inner companion is below the hydrogen-burning limit; however, the true mass is likely to be substantially higher. We are able to exclude transits of the inner companion with high confidence. Further, the host star spectrum exhibits a clear signature of Ca H and K core emission, indicating stellar activity, but a lack of photometric variability and small v sin I suggest that the primary's spin axis is oriented in a pole-on configuration. The rotational period of the primary estimated through an activity-rotation relation matches the orbital period of the inner companion to within 1.5 sigma, suggesting that the primary and inner companion are tidally locked. If the inner companion's orbital angular momentum vector is aligned with the stellar spin axis as expected through tidal evolution, then it has a stellar mass of similar to 0.3-0.4 M-circle dot. Direct imaging limits the existence of stellar companions to projected separations <30 AU. No set of spectral lines and no significant flux contribution to the SED from either companion are detected, which places individual upper mass limits of M-{2,M-3} less than or similar to 1.0 M-circle dot, provided they are not stellar remnants. If the tertiary is not a stellar remnant, then it likely has a mass of similar to 0.5-0.6M(circle dot), and its orbit is likely significantly inclined from that of the secondary, suggesting that the Kozai-Lidov mechanism may have driven the dynamical evolution of this system.

引用

页数：19

共 5 条

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