Close Companions around Young Stars

Multiplicity is a fundamental property that is set early during stellar lifetimes, and it is a stringent probe of the physics of star formation. The distribution of close companions around young stars is still poorly constrained by observations. We present an analysis of stellar multiplicity derived...

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Bibliographic Details
Published in:The Astronomical journal 2019-05, Vol.157 (5), p.196
Main Authors: Kounkel, Marina, Covey, Kevin, Moe, Maxwell, Kratter, Kaitlin M., Suárez, Genaro, Stassun, Keivan G., Román-Zúñiga, Carlos, Hernandez, Jesus, Kim, Jinyoung Serena, Ramírez, Karla Peña, Roman-Lopes, Alexandre, Stringfellow, Guy S, Jaehnig, Karl O, Borissova, Jura, Tofflemire, Benjamin, Krolikowski, Daniel, Rizzuto, Aaron, Kraus, Adam, Badenes, Carles, Longa-Peña, Penélope, Maqueo Chew, Yilen Gómez, Barba, Rodolfo, Nidever, David L., Brown, Cody, De Lee, Nathan, Pan, Kaike, Bizyaev, Dmitry, Oravetz, Daniel, Oravetz, Audrey
Format: Article
Language:English
Subjects:
Astronomy
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
binaries: spectroscopic
Companion stars
DENSITY
Disks
Dispersal
DISTRIBUTION
GALACTIC EVOLUTION
MAIN SEQUENCE STARS
MASS
MULTIPLICITY
RADIAL VELOCITY
RESOLUTION
SPECTRA
Star & galaxy formation
Star formation
stars: pre-main sequence
Stellar evolution
System effectiveness
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Summary:Multiplicity is a fundamental property that is set early during stellar lifetimes, and it is a stringent probe of the physics of star formation. The distribution of close companions around young stars is still poorly constrained by observations. We present an analysis of stellar multiplicity derived from Apache Point Observatory Galactic Evolution Experiment-2 spectra obtained in targeted observations of nearby star-forming regions. This is the largest homogeneously observed sample of high-resolution spectra of young stars. We developed an autonomous method to identify double-lined spectroscopic binaries (SB2s). Out of 5007 sources spanning the mass range of ∼0.05-1.5 M , we find 399 binaries, including both radial velocity (RV) variables and SB2s. The mass ratio distribution of SB2s is consistent with being uniform for q < 0.95 with an excess of twins for q > 0.95. The period distribution is consistent with what has been observed in close binaries (
ISSN:0004-6256
1538-3881
1538-3881
DOI:10.3847/1538-3881/ab13b1