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Very low mass stellar and substellar companions to solar-like stars from MARVELS. I. A low-mass ratio stellar companion to TYC 4110-01037-1 in a 79 day orbit

By J.P. Wisniewski, Jian Ge, Justin R. Crepp, Nathan M. De Lee, Jason Eastman, Massimiliano Esposito, S.W. Fleming, B. S. Gaudi, Luan Ghezzi, Jonay I. González Hernández, Brian L. Lee, Keivan G. Stassun, Eric Agol, Carlos Allende Prieto, Rory Barnes, D. Bizyaev, Phillip A. Cargile, Liang Chang, Luiz N. da Costa, Gustavo Frederico Porto de Mello, B. Femenía Castellá, Letícia D. Ferreira, Bruce L. Gary, Leslie Hebb, J.A. Holtzman, Jian Liu, Bo Ma, C. E. Mack, Suvrath Mahadevan, Marcio Antonio Geimba Maia, D.C. Nguyen, Ricardo L.C. Ogando, Daniel J. Oravetz, Martin Paegert, K. Pan, J. Pepper, Rafael Rebolo, Basilio Xavier Santiago, D.P. Schneider, Alaina C. Shelden Bradley, Audrey E. Simmons, Benjamin M. Tofflemire, Xiaoke Wan, Ji Wang and Bo Zhao

Abstract

TYC 4110-01037-1 has a low-mass stellar companion, whose small mass ratio and short orbital period are atypical among binary systems with solar-like (Teff 6000 K) primary stars. Our analysis of TYC 4110-01037-1 reveals it to be a moderately aged ( 5 Gyr) solar-like star having a mass of 1.07 ± 0.08M and radius of 0.99 ± 0.18 R . We analyze 32 radial velocity (RV) measurements from the SDSS-III MARVELS survey as well as 6 supporting RV measurements from the SARG spectrograph on the 3.6 m Telescopio Nazionale Galileo telescope obtained over a period of ∼2 years. The best Keplerian orbital fit parameters were found to have a period of 78.994 ± 0.012 days, an eccentricity of 0.1095 ± 0.0023, and a semi-amplitude of 4199 ± 11 m s−1. We determine the minimum companion mass (if sin i = 1) to be 97.7 ± 5.8 MJup. The system’s companion to host star mass ratio, 0.087 ± 0.003, places it at the lowest end of observed values for short period stellar companions to solar-like (Teff 6000 K) stars. One possible way to create such a system would be if a triple-component stellar multiple broke up into a short period, low q binary during the cluster dispersal phase of its lifetime. A candidate tertiary body has been identified in the system via single-epoch, high contrast imagery. If this object is confirmed to be comoving, we estimate it would be a dM4 star. We present these results in the context of our larger-scale effort to constrain the statistics of low-mass stellar and brown dwarf companions to FGK-type stars via the MARVELS survey

Topics: Estrelas binarias, Binaries: general, Stars: individual (TYC 4110-01037-1), Mecanica celeste, Anãs marrons, Stars: low mass, Massa estelar, Movimento estelar
Year: 2014
OAI identifier: oai:agregador.ibict.br.PC_UFRGS:oai:www.lume.ufrgs.br:10183/108139
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