Astrometry and Precise Radial Velocities Yield a Complete Orbital Solution for the Nearby Eccentric Brown Dwarf LHS 1610 b
Fuente:
arXiv
Guardado en:
| Autores principales: | , , , , , , , , , , , , , , , , , , , , |
|---|---|
| Formato: | Preprint |
| Publicado: |
2023
|
| Materias: | |
| Acceso en línea: | |
| Etiquetas: |
Agregar Etiqueta
Sin Etiquetas, Sea el primero en etiquetar este registro!
|
| _version_ | 1866908273303617536 |
|---|---|
| author | Fitzmaurice, Evan Stefánsson, Gudmundur Kavanagh, Robert D. Mahadevan, Suvrath Cañas, Caleb I. Winn, Joshua N. Robertson, Paul Ninan, Joe P. Albrecht, Simon Callingham, J. R. Cochran, William D. Delamer, Megan Ford, Eric B. Kanodia, Shubham Lin, Andrea S. J. Marcussen, Marcus L. Pope, Benjamin J. S. Ramsey, Lawrence W. Roy, Arpita Vedantham, Harish Wright, Jason T. |
| author_facet | Fitzmaurice, Evan Stefánsson, Gudmundur Kavanagh, Robert D. Mahadevan, Suvrath Cañas, Caleb I. Winn, Joshua N. Robertson, Paul Ninan, Joe P. Albrecht, Simon Callingham, J. R. Cochran, William D. Delamer, Megan Ford, Eric B. Kanodia, Shubham Lin, Andrea S. J. Marcussen, Marcus L. Pope, Benjamin J. S. Ramsey, Lawrence W. Roy, Arpita Vedantham, Harish Wright, Jason T. |
| contents | The LHS 1610 system consists of a nearby ($d=9.7$ pc) M5 dwarf hosting a candidate brown dwarf companion in a $10.6$ day, eccentric ($e \sim 0.37$) orbit. We confirm this brown dwarf designation and estimate its mass ($ 49.5_{-3.5}^{+4.3}$ $M_{\text{Jup}} $) and inclination ($ 114.5^\circ$ $_{-10.0}^{+7.4}$) by combining discovery radial velocities (RVs) from TRES and new RVs from the Habitable-zone Planet Finder with the available Gaia astrometric two-body solution. We highlight a discrepancy between the measurement of the eccentricity from the Gaia two-body solution ($e=0.52 \pm 0.03$) and the RV-only solution ($e=0.3702\pm0.0003$). We discuss possible reasons for this discrepancy, which can be further probed when the Gaia astrometric time series becomes available as part of Gaia DR4. As a nearby mid-M star hosting a massive short-period companion with a well-characterized orbit, LHS 1610 b is a promising target to look for evidence of sub-Alfvénic interactions and/or auroral emission at optical and radio wavelengths. LHS 1610 has a flare rate ($0.28\pm 0.07$ flares/day) on the higher-end for its rotation period ($84 \pm 8$ days), similar to other mid-M dwarf systems such as Proxima Cen and YZ Ceti that have recent radio detections compatible with star-planet interactions. While available TESS photometry is insufficient to determine an orbital phase-dependence of the flares, our complete orbital characterization of this system makes it attractive to probe star-companion interactions with additional photometric and radio observations. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2310_07827 |
| institution | arXiv |
| publishDate | 2023 |
| record_format | arxiv |
| spellingShingle | Astrometry and Precise Radial Velocities Yield a Complete Orbital Solution for the Nearby Eccentric Brown Dwarf LHS 1610 b Fitzmaurice, Evan Stefánsson, Gudmundur Kavanagh, Robert D. Mahadevan, Suvrath Cañas, Caleb I. Winn, Joshua N. Robertson, Paul Ninan, Joe P. Albrecht, Simon Callingham, J. R. Cochran, William D. Delamer, Megan Ford, Eric B. Kanodia, Shubham Lin, Andrea S. J. Marcussen, Marcus L. Pope, Benjamin J. S. Ramsey, Lawrence W. Roy, Arpita Vedantham, Harish Wright, Jason T. Solar and Stellar Astrophysics Earth and Planetary Astrophysics The LHS 1610 system consists of a nearby ($d=9.7$ pc) M5 dwarf hosting a candidate brown dwarf companion in a $10.6$ day, eccentric ($e \sim 0.37$) orbit. We confirm this brown dwarf designation and estimate its mass ($ 49.5_{-3.5}^{+4.3}$ $M_{\text{Jup}} $) and inclination ($ 114.5^\circ$ $_{-10.0}^{+7.4}$) by combining discovery radial velocities (RVs) from TRES and new RVs from the Habitable-zone Planet Finder with the available Gaia astrometric two-body solution. We highlight a discrepancy between the measurement of the eccentricity from the Gaia two-body solution ($e=0.52 \pm 0.03$) and the RV-only solution ($e=0.3702\pm0.0003$). We discuss possible reasons for this discrepancy, which can be further probed when the Gaia astrometric time series becomes available as part of Gaia DR4. As a nearby mid-M star hosting a massive short-period companion with a well-characterized orbit, LHS 1610 b is a promising target to look for evidence of sub-Alfvénic interactions and/or auroral emission at optical and radio wavelengths. LHS 1610 has a flare rate ($0.28\pm 0.07$ flares/day) on the higher-end for its rotation period ($84 \pm 8$ days), similar to other mid-M dwarf systems such as Proxima Cen and YZ Ceti that have recent radio detections compatible with star-planet interactions. While available TESS photometry is insufficient to determine an orbital phase-dependence of the flares, our complete orbital characterization of this system makes it attractive to probe star-companion interactions with additional photometric and radio observations. |
| title | Astrometry and Precise Radial Velocities Yield a Complete Orbital Solution for the Nearby Eccentric Brown Dwarf LHS 1610 b |
| topic | Solar and Stellar Astrophysics Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2310.07827 |