Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003mnras.342..564v&link_type=abstract
Monthly Notice of the Royal Astronomical Society, Volume 342, Issue 2, pp. 564-574.
Astronomy and Astrophysics
Astronomy
4
Stars: Activity, Binaries: Close, Stars: Magnetic Fields, Stars: Spots, Stars: Winds, Outflows
Scientific paper
The eclipsing binary FF Aquarii (FF Aqr) consists of a small hot star of uncertain type and a red giant. An Hα feature varies from absorption during eclipse to maximum emission during hot star transit. We have obtained simultaneous differential photometry in BVRI bands and Hα spectroscopy in 1998 that covered an entire orbit with some overlap. A binary star model was used with our light-curve, radial velocity and Hα data to refine stellar and orbital parameters. A new ephemeris indicates that the period has increased or is longer than previously thought. A physically simple algorithm is developed that generates properly blended spectral line profiles of binaries with arbitrary combinations of surface emission and absorption line regions. Although there is no radiative transfer, the algorithm can accommodate modest geometrical intricacy. For now, all line broadening in the model is rotational. The algorithm has now been incorporated within the general Wilson-Devinney binary star model, and we used it to model FF Aqr's photospheric iron profile. It also is used to generate templates that illustrate problems with FF Aqr's strongly time-dependent Hα emission profiles, which appear to be blends of features from the photosphere and from above the photosphere. The dominant broadening mechanism should be rotation for individual line components. Absorption profiles were generated by the model and fit to the observations to yield a red star radius ~6.9 Rsolar, which then requires i~ 76°. Our light-curve models have five spots with temperatures ~1000 K cooler than the surrounding photosphere. Hα emission was modelled on the red star surface, centred at the substellar point to simulate a fluorescent chromosphere. Additional emission is seen outside our modelled profiles. The origins of this excess emission may be corotating prominences, winds, or coronal mass ejections, all of which could affect the orbit period.
Vaccaro Todd Russell
Wilson Robert E.
No associations
LandOfFree
Fluorescence in ultraviolet active binaries: the case of FF Aquarii does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Fluorescence in ultraviolet active binaries: the case of FF Aquarii, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Fluorescence in ultraviolet active binaries: the case of FF Aquarii will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1526317