Bibcode
Wisniewski, John P.; Ge, Jian; Crepp, Justin R.; De Lee, Nathan; Eastman, Jason; Esposito, M.; Fleming, Scott W.; Gaudi, B. Scott; Ghezzi, Luan; Gonzalez-Hernandez, J. I.; Lee, Brian L.; Stassun, Keivan G.; Agol, Eric; Allende-Prieto, C.; Barnes, Rory; Bizyaev, Dmitry; Cargile, Phillip; Chang, Liang; Da Costa, Luiz N.; Porto De Mello, G. F.; Femenía, B.; Ferreira, Leticia D.; Gary, Bruce; Hebb, Leslie; Holtzman, Jon; Liu, Jian; Ma, Bo; Mack, Claude E.; Mahadevan, Suvrath; Maia, Marcio A. G.; Nguyen, Duy Cuong; Ogando, Ricardo L. C.; Oravetz, Daniel J.; Paegert, Martin; Pan, Kaike; Pepper, Joshua; Rebolo, R.; Santiago, Basilio; Schneider, Donald P.; Shelden, Alaina C.; Simmons, Audrey; Tofflemire, Benjamin M.; Wan, Xiaoke; Wang, Ji; Zhao, Bo
Bibliographical reference
The Astronomical Journal, Volume 143, Issue 5, article id. 107 (2012).
Advertised on:
5
2012
Citations
23
Refereed citations
23
Description
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 (T eff <~ 6000 K) primary stars. Our analysis
of TYC 4110-01037-1 reveals it to be a moderately aged (lsim5 Gyr)
solar-like star having a mass of 1.07 ± 0.08 M &sun;
and radius of 0.99 ± 0.18 R &sun;. 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 M Jup. 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 (T
eff <~ 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.
Related projects
Very Low Mass Stars, Brown Dwarfs and Planets
Our goal is to study the processes that lead to the formation of low mass stars, brown dwarfs and planets and to characterize the physical properties of these objects in various evolutionary stages. Low mass stars and brown dwarfs are likely the most numerous type of objects in our Galaxy but due to their low intrinsic luminosity they are not so
Rafael
Rebolo López
Observational Tests of the Processes of Nucleosynthesis in the Universe
Several spectroscopic analyses of stars with planets have recently been carried out. One of the most remarkable results is that planet-harbouring stars are on average more metal-rich than solar-type disc stars. Two main explanations have been suggested to link this metallicity excess with the presence of planets. The first of these, the “self
Garik
Israelian