English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Tools annual

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

The aims of our study are to improve the orbital elements of the giant and toderive the spectroscopic orbit for the white dwarf companion. Spectralvariations related to the 2006 outburst are also studied. The spectroscopicorbits have been obtained by measuring the radial velocities of the coolcomponent absorption lines and the broad Halpha emission wings, which seem tobe associated with the hot component. A set of cF-type absorption lines werealso analyzed for a possible connection with the hot component motion. A newperiod of 453.6 days and a mass ratio, q=M_g/M_h=0.59 were determined. Assuminga massive white dwarf as the hot component, M_h= 1.2-1.4 M_{\odot}, the redgiant mass is M_g= 0.68-0.80 M_{\odot} and the orbit inclination, i =49-52^{\circ}. The cF-type lines are not associated with either binarycomponent, and are most likely formed in the material streaming towards the hotcomponent. We also confirm the presence of the LiI doublet in RS Oph and itsradial velocities fit very well the M-giant radial velocity curve. Regardlessof the mechanism involved to produce lithium, its origin is most likely fromwithin the cool giant rather than material captured by the giant at the time ofthe nova explosion. In April 2006 most of the emission lines present a broadpedestal with a strong and narrow component at about -20 km/s and two otherextended emission components at -200 and +150 km/s. These components couldoriginate in a bipolar gas outflow supporting the model of a bipolarshock-heated shell expanding through the cool component wind perpendicularly tothe binary orbital plane.

Spectroscopic orbits and variations of RS Oph