DQ Tau
(young binary star system)
DQ Tau is a non-eclipsing double-line spectroscopic binary
of young T-Tauri stars, each on the order of 0.65 solar masses,
about 140 parsecs distant. They have a
highly-eccentric orbit in which their nearest
encounter (periastron) is slightly above 8 radii of either star,
with an orbital period of 16 days.
The star system has been studied for X-ray emissions
attributed to the orbit's effect on their colliding
magnetospheres.
(star,binary star,magnetosphere,eccentricity,variable star,PMS star,TTS)
Further reading:
http://simbad.u-strasbg.fr/simbad/sim-id?Ident=DQ%20Tau
https://webdisks.jpl.nasa.gov/show.php?id=35&name=DQ%20Tau
https://ui.adsabs.harvard.edu/abs/2001IAUS..200..415S/abstract
https://ui.adsabs.harvard.edu/abs/2011ApJ...730....6G/abstract
https://ui.adsabs.harvard.edu/abs/2022ApJ...928...81F/abstract
Redshift | Parsecs /Distance | Lightyears /Lookback Years | | |
~0 | 140pc | 460ly | | DQ Tau |
|
Coordinates: | DQ Tau J044653.06+170000.1 |
|
Referenced by pages:
variable star
variable star designation
Index