Follow Us| V3885 Sgr | ||||||||||||||||||
| The FUSE spectrum of the nova-like V3885 Sgr is shown with a WD+disk model fit including the contribution from a hot boundary layer. The 0.7 solar mass WD model has a temperature of 60,000K, a projected rotational velocity of 200 km/s, and solar abundances. The disk model has a mass accretion rate of 3.E-9 solar mass per year with an inclination of 60deg and includes two inner (boundary layer) rings with T=175,000K. The WD (dotted line) contributes only 22% of the flux and the disk+BL (dashed line) contributes 78%. The sharp absorption lines are from the ISM. All the broad absorption lines originate from a corona above the disk and/or boundary layer and are blue shifted by 1-1.5A. The lines are all marked at their rest wavelengths to emphasize the shift. All the absorption lines are colored in blue and only the continuum (in red) is modeled. | |||||||||||||||||
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FUSE Data
Synthetic Spectrum
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These data and models were published in the paper:
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Notes on figures:The flux (vertical axis) is given in ergs/sec/cm2/A and the wavelength (horizontal axis) is given in Angstroem. For clarity the spectrum is shown on 3 panels: the upper panel from about 900 to 1000A, the middle panel from about 1000A to 1100A, and the lower panel from about 1100A to 1200A. Air glow emission is anoted above each panel with a "+" sign inside a circle. Strong emission lines reaching the upper part of the frame in each pael is marked just above the panel. The Hydrogen series is marked below the x-axis in the upper and middle panel and the hydrogen cut-off limit is clearly marked around 915A with an increasing density of tick marks. The He I (1168A) is marked below the lower panel. Oxygen I lines are shown with an arrow "OI -->" if many (ISM) OI lines are present, they are just annotated with verical tick marks in the lower portion of each panel. ISM molecular hydrogen lines are either individually annotated vertically (e.g. L10R1) or just marked with an arrow "MH -->" and vertical tick marks (usually in the upper part of each panel). Features resulting from fixed pattern noise introduced by FUSE detect ors are indicated with "FPN;.When a model is shown, the portions of the observed spectrum that have been masked before the spectral fit are in blue, while the rest of the observed spectrum is in red. The model fit is shown the solide line in black (or possibly white). If the model is a composite made of a disk model and a white dwarf model, then these are shown with the dashed- and dotted lines (respectively). Some models include the effect of quasi-molecular HI absorption features, these are labelled "Q-mol" in the spectrum. |
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