Star-crossed Lovers DI Tau A and B: Orbit Characterization and Physical Properties Determination
The stellar companion to the weak-line T Tauri star DI Tau A was first discovered by the lunar occultation technique in 1989 and was subsequently confirmed by a speckle imaging observation in 1991. It has not been detected since, despite being targeted by five different studies that used a variety o...
| Main Authors: | , , , , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/acc58b |
| _version_ | 1827829979284504576 |
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| author | Shih-Yun Tang Asa G. Stahl L. Prato G. H. Schaefer Christopher M. Johns-Krull Brian A. Skiff Charles A. Beichman Taichi Uyama |
| author_facet | Shih-Yun Tang Asa G. Stahl L. Prato G. H. Schaefer Christopher M. Johns-Krull Brian A. Skiff Charles A. Beichman Taichi Uyama |
| author_sort | Shih-Yun Tang |
| collection | DOAJ |
| description | The stellar companion to the weak-line T Tauri star DI Tau A was first discovered by the lunar occultation technique in 1989 and was subsequently confirmed by a speckle imaging observation in 1991. It has not been detected since, despite being targeted by five different studies that used a variety of methods and spanned more than 20 yr. Here, we report the serendipitous rediscovery of DI Tau B during our Young Exoplanets Spectroscopic Survey (YESS). Using radial velocity data from YESS spanning 17 yr, new adaptive optics observations from Keck II, and a variety of other data from the literature, we derive a preliminary orbital solution for the system that effectively explains the detection and (almost all of the) non-detection history of DI Tau B. We estimate the dynamical masses of both components, finding that the large mass difference ( q ∼ 0.17) and long orbital period (≳35 yr) make the DI Tau system a noteworthy and valuable addition to studies of stellar evolution and pre-main-sequence models. With a long orbital period and a small flux ratio (f2/f1) between DI Tau A and B, additional measurements are needed for a better comparison between these observational results and pre-main-sequence models. Finally, we report an average surface magnetic field strength ( $\bar{B}$ ) for DI Tau A, of ∼0.55 kG, which is unusually low in the context of young active stars. |
| first_indexed | 2024-03-12T04:14:08Z |
| format | Article |
| id | doaj.art-994706f3c22b4c14860ee4ad4a575088 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-12T04:14:08Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-994706f3c22b4c14860ee4ad4a5750882023-09-03T10:48:19ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-0195029210.3847/1538-4357/acc58bStar-crossed Lovers DI Tau A and B: Orbit Characterization and Physical Properties DeterminationShih-Yun Tang0https://orcid.org/0000-0003-4247-1401Asa G. Stahl1https://orcid.org/0000-0002-0848-6960L. Prato2https://orcid.org/0000-0001-7998-226XG. H. Schaefer3https://orcid.org/0000-0001-5415-9189Christopher M. Johns-Krull4https://orcid.org/0000-0002-8828-6386Brian A. Skiff5https://orcid.org/0000-0001-5306-6220Charles A. Beichman6https://orcid.org/0000-0002-5627-5471Taichi Uyama7https://orcid.org/0000-0002-6879-3030Lowell Observatory , 1400 West Mars Hill Road, Flagstaff, AZ 86001, USA ; sytang@lowell.edu, Asa.Stahl@rice.edu; Department of Physics and Astronomy, Rice University , 6100 Main Street, Houston, TX 77005, USA; Department of Astronomy and Planetary Science, Northern Arizona University , Flagstaff, AZ 86011, USADepartment of Physics and Astronomy, Rice University , 6100 Main Street, Houston, TX 77005, USALowell Observatory , 1400 West Mars Hill Road, Flagstaff, AZ 86001, USA ; sytang@lowell.edu, Asa.Stahl@rice.eduThe CHARA Array of Georgia State University , Mount Wilson Observatory, Mount Wilson, CA 91023, USADepartment of Physics and Astronomy, Rice University , 6100 Main Street, Houston, TX 77005, USALowell Observatory , 1400 West Mars Hill Road, Flagstaff, AZ 86001, USA ; sytang@lowell.edu, Asa.Stahl@rice.eduInfrared Processing and Analysis Center, California Institute of Technology , 1200 E. California Boulevard, Pasadena, CA 91125, USA; NASA Exoplanet Science Institute , Pasadena, CA 91125, USAInfrared Processing and Analysis Center, California Institute of Technology , 1200 E. California Boulevard, Pasadena, CA 91125, USA; NASA Exoplanet Science Institute , Pasadena, CA 91125, USA; National Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanThe stellar companion to the weak-line T Tauri star DI Tau A was first discovered by the lunar occultation technique in 1989 and was subsequently confirmed by a speckle imaging observation in 1991. It has not been detected since, despite being targeted by five different studies that used a variety of methods and spanned more than 20 yr. Here, we report the serendipitous rediscovery of DI Tau B during our Young Exoplanets Spectroscopic Survey (YESS). Using radial velocity data from YESS spanning 17 yr, new adaptive optics observations from Keck II, and a variety of other data from the literature, we derive a preliminary orbital solution for the system that effectively explains the detection and (almost all of the) non-detection history of DI Tau B. We estimate the dynamical masses of both components, finding that the large mass difference ( q ∼ 0.17) and long orbital period (≳35 yr) make the DI Tau system a noteworthy and valuable addition to studies of stellar evolution and pre-main-sequence models. With a long orbital period and a small flux ratio (f2/f1) between DI Tau A and B, additional measurements are needed for a better comparison between these observational results and pre-main-sequence models. Finally, we report an average surface magnetic field strength ( $\bar{B}$ ) for DI Tau A, of ∼0.55 kG, which is unusually low in the context of young active stars.https://doi.org/10.3847/1538-4357/acc58bBinary starsVisual binary starsPre-main sequence starsRadial velocityHigh angular resolutionFundamental parameters of stars |
| spellingShingle | Shih-Yun Tang Asa G. Stahl L. Prato G. H. Schaefer Christopher M. Johns-Krull Brian A. Skiff Charles A. Beichman Taichi Uyama Star-crossed Lovers DI Tau A and B: Orbit Characterization and Physical Properties Determination The Astrophysical Journal Binary stars Visual binary stars Pre-main sequence stars Radial velocity High angular resolution Fundamental parameters of stars |
| title | Star-crossed Lovers DI Tau A and B: Orbit Characterization and Physical Properties Determination |
| title_full | Star-crossed Lovers DI Tau A and B: Orbit Characterization and Physical Properties Determination |
| title_fullStr | Star-crossed Lovers DI Tau A and B: Orbit Characterization and Physical Properties Determination |
| title_full_unstemmed | Star-crossed Lovers DI Tau A and B: Orbit Characterization and Physical Properties Determination |
| title_short | Star-crossed Lovers DI Tau A and B: Orbit Characterization and Physical Properties Determination |
| title_sort | star crossed lovers di tau a and b orbit characterization and physical properties determination |
| topic | Binary stars Visual binary stars Pre-main sequence stars Radial velocity High angular resolution Fundamental parameters of stars |
| url | https://doi.org/10.3847/1538-4357/acc58b |
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