GK Tauri is a young binary system composed of T Tauri-type pre-main sequence stars in the constellation of Taurus about 466 light years away, belonging to the Taurus Molecular Cloud. In 1978, Jonathan H. Elias announced that the object, then known as Haro 6-10, is a variable star, based on near infrared observations made from 1975 through 1978.
System The stars GV Tauri A (GV Tauri S) and G Tauri B (GV Tauri N) form a wide binary system, with the projected separation between components being 170 AU. Both are strongly shrouded by circumstellar dust - GV Tauri A by 30 magnitudes and the GV Tauri B up to 59 magnitudes in the V band. Both components are suspected to be binaries themselves, as they produce strongly ionized jets and molecular outflows.
Properties Both members of the binary system are medium-mass objects still contracting towards the main sequence and accreting mass, although accretion rates remain highly uncertain as of 2009.
Protoplanetary system Both stars are surrounded by protoplanetary disks, with the observable dust in each being about 5×10−5 M☉, and the gas about 0.005 M☉. The disk of GV Tauri B is rich in carbon monoxide, hydrogen cyanide and, unusually, methane.
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