Rotational Velocities and Radii Estimates of Low-mass Pre-main-sequence Stars in NGC 2264
Investigating the angular momentum evolution of pre-main-sequence (PMS) stars provides important insight into the interactions between Sun-like stars and their protoplanetary disks, and the timescales that govern disk dissipation and planet formation. We present projected rotational velocities ( v s...
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2024-01-01
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| Online Access: | https://doi.org/10.3847/1538-4357/ad924b |
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| author | Laurin M. Gray Katherine L. Rhode Catrina M. Hamilton-Drager Tiffany Picard Luisa M. Rebull |
| author_facet | Laurin M. Gray Katherine L. Rhode Catrina M. Hamilton-Drager Tiffany Picard Luisa M. Rebull |
| author_sort | Laurin M. Gray |
| collection | DOAJ |
| description | Investigating the angular momentum evolution of pre-main-sequence (PMS) stars provides important insight into the interactions between Sun-like stars and their protoplanetary disks, and the timescales that govern disk dissipation and planet formation. We present projected rotational velocities ( v sin i values) of 254 T Tauri stars (TTSs) in the ∼3 Myr old open cluster NGC 2264, measured using high-dispersion spectra from the WIYN 3.5 m telescope’s Hydra instrument. We combine these with literature values of temperature, rotation period, luminosity, disk classification, and binarity. We find some evidence that weak-lined TTSs may rotate faster than their classical TTS counterparts and that stars in binary systems may rotate faster than single stars. We also combine our v sin i measurements with rotation period to estimate the projected stellar radii of our sample stars, and then use a maximum likelihood modeling technique to compare our radii estimates to predicted values from stellar evolution models. We find that starspot-free models tend to underestimate the radii of the PMS stars at the age of the cluster, while models that incorporate starspots are more successful. We also observe a mass dependence in the degree of radius inflation, which may be a result of differences in the birth-line location on the HR diagram. Our study of NGC 2264 serves as a pilot study for analysis methods to be applied to four other clusters ranging in age from 1−14 Myr, which is the timescale over which protoplanetary disks dissipate and planetary systems begin to form. |
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| language | English |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
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| spelling | doaj-art-c52ac19614fd4eefb00d51177ec07bf62025-08-20T02:37:10ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-01977227010.3847/1538-4357/ad924bRotational Velocities and Radii Estimates of Low-mass Pre-main-sequence Stars in NGC 2264Laurin M. Gray0https://orcid.org/0000-0001-6389-5639Katherine L. Rhode1https://orcid.org/0000-0001-8283-4591Catrina M. Hamilton-Drager2https://orcid.org/0000-0001-5924-3531Tiffany Picard3Luisa M. Rebull4https://orcid.org/0000-0001-6381-515XDepartment of Astronomy, Indiana University , 727 East Third Street, Bloomington, IN 47405, USA ; grayla@iu.eduDepartment of Astronomy, Indiana University , 727 East Third Street, Bloomington, IN 47405, USA ; grayla@iu.eduDepartment of Physics and Astronomy, Dickinson College , 28 N. College Street, Carlisle, PA 17013, USAAstronomy Department, Mount Holyoke College , 50 College Street, South Hadley, MA 01075, USAInfrared Science Archive (IRSA), IPAC, California Institute of Technology , 1200 E. California Boulevard, Pasadena, CA 91125, USAInvestigating the angular momentum evolution of pre-main-sequence (PMS) stars provides important insight into the interactions between Sun-like stars and their protoplanetary disks, and the timescales that govern disk dissipation and planet formation. We present projected rotational velocities ( v sin i values) of 254 T Tauri stars (TTSs) in the ∼3 Myr old open cluster NGC 2264, measured using high-dispersion spectra from the WIYN 3.5 m telescope’s Hydra instrument. We combine these with literature values of temperature, rotation period, luminosity, disk classification, and binarity. We find some evidence that weak-lined TTSs may rotate faster than their classical TTS counterparts and that stars in binary systems may rotate faster than single stars. We also combine our v sin i measurements with rotation period to estimate the projected stellar radii of our sample stars, and then use a maximum likelihood modeling technique to compare our radii estimates to predicted values from stellar evolution models. We find that starspot-free models tend to underestimate the radii of the PMS stars at the age of the cluster, while models that incorporate starspots are more successful. We also observe a mass dependence in the degree of radius inflation, which may be a result of differences in the birth-line location on the HR diagram. Our study of NGC 2264 serves as a pilot study for analysis methods to be applied to four other clusters ranging in age from 1−14 Myr, which is the timescale over which protoplanetary disks dissipate and planetary systems begin to form.https://doi.org/10.3847/1538-4357/ad924bYoung stellar objectsPre-main sequence starsT Tauri starsClassical T Tauri starsWeak-line T Tauri starsStellar rotation |
| spellingShingle | Laurin M. Gray Katherine L. Rhode Catrina M. Hamilton-Drager Tiffany Picard Luisa M. Rebull Rotational Velocities and Radii Estimates of Low-mass Pre-main-sequence Stars in NGC 2264 The Astrophysical Journal Young stellar objects Pre-main sequence stars T Tauri stars Classical T Tauri stars Weak-line T Tauri stars Stellar rotation |
| title | Rotational Velocities and Radii Estimates of Low-mass Pre-main-sequence Stars in NGC 2264 |
| title_full | Rotational Velocities and Radii Estimates of Low-mass Pre-main-sequence Stars in NGC 2264 |
| title_fullStr | Rotational Velocities and Radii Estimates of Low-mass Pre-main-sequence Stars in NGC 2264 |
| title_full_unstemmed | Rotational Velocities and Radii Estimates of Low-mass Pre-main-sequence Stars in NGC 2264 |
| title_short | Rotational Velocities and Radii Estimates of Low-mass Pre-main-sequence Stars in NGC 2264 |
| title_sort | rotational velocities and radii estimates of low mass pre main sequence stars in ngc 2264 |
| topic | Young stellar objects Pre-main sequence stars T Tauri stars Classical T Tauri stars Weak-line T Tauri stars Stellar rotation |
| url | https://doi.org/10.3847/1538-4357/ad924b |
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