Geometry of the Draco C1 Symbiotic Binary

• Published in: arXiv.org
• Main Authors: Lewis, Hannah M, Anguiano, Borja, Stassun, Keivan G, Majewski, Steven R, Arras, Phil, Sarazin, Craig L, Zhi-Yun, Li, De Lee, Nathan, Troup, Nicholas W, Carlos Allende Prieto, Badenes, Carles, Cunha, Katia, Garcia-Hernandez, D A, Nidever, David L, Palicio, Pedro A, Simon, Joshua D, Smith, Verne V
• Format: Paper Journal Article
• Language: English
• Published: Ithaca Cornell University Library, arXiv.org 18.09.2020
• Subjects: Binary stars; Companion stars; Deposition; Dwarf galaxies; Galactic evolution; Infrared spectra; Near infrared radiation; Orbits; Parameters; Periodic variations; Physics - Astrophysics of Galaxies; Physics - Solar and Stellar Astrophysics; Radial velocity; Red giant stars; Sky surveys (astronomy); Spheroidal galaxies; Stellar winds; White dwarf stars
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.2008.05962

Draco C1 is a known symbiotic binary star system composed of a carbon red giant and a hot, compact companion -- likely a white dwarf -- belonging to the Draco dwarf spheroidal galaxy. From near-infrared spectroscopic observations taken by the Apache Point Observatory Galactic Evolution Experiment (APOGEE-2), part of Sloan Digital Sky Survey IV, we provide updated stellar parameters for the cool, giant component, and constrain the temperature and mass of the hot, compact companion. Prior measurements of the periodicity of the system, based on only a few epochs of radial velocity data or relatively short baseline photometric observations, were sufficient only to place lower limits on the orbital period (\(P > 300\) days). For the first time, we report precise orbital parameters for the binary system: With 43 radial velocity measurements from APOGEE spanning an observational baseline of more than 3 years, we definitively derive the period of the system to be \(1220.0^{+3.7}_{-3.5}\) days. Based on the newly derived orbital period and separation of the system, together with estimates of the radius of the red giant star, we find that the hot companion must be accreting matter from the dense wind of its evolved companion.