Open AccessThe disc evolution of V2051 Oph on decline from superoutburst
Author(s) -
Vrielmann Sonja,
Offutt Warren
Publication year - 2003
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2003.06030.x
Subject(s) - physics , dwarf nova , astrophysics , precession , accretion disc , brightness , eclipse , light curve , accretion (finance) , astronomy , white dwarf , stars
We present an Eclipse Mapping analysis of ten eclipses taken during decline from superoutburst of the dwarf nova V2051 Oph. On decline from superoutburst the disc cools down considerably from nearly 50 000 K in the intermediate disc (∼0.2 R L1 ) near maximum to about 25 000 K at the end of our observing run, i.e. within four days. The average mass accretion rate through the disc drops in the same time from 10 18 g s −1 to below 10 17 g s −1 . While in some maps the brightness temperature follows the steady‐state model, in others the temperature profile shows flattenings and/or an indication of an inward travelling cooling front with a speed of approximately −0.12 km s −1 , possibly a reflected heating front with a speed of +1.8 km s −1 and a newly reflected cooling front with the same speed as the first. Such a scenario has been predicted but has not been observed before. Furthermore, we see a prograde precession of the enlarged disc with a precession period of about 52.5 h in very good agreement with the independently determined superhump period observed by Kiyota and Kato. At the same time, the uneclipsed component – presumably a disc wind – decreases significantly in strength during decline from superoutburst.