On the nature of the outburst stage in the symbiotic binary AX Persei

Details On the nature of the outburst stage in the symbiotic binary AX Persei On the nature of the outburst stage in the symbiotic binary AX Persei

Jun 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...286..453s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 286, no. 2, p. 453-462

Astronomy and Astrophysics

Astrophysics

15

Eclipsing Binary Stars, Light Curve, Line Spectra, Red Giant Stars, Stellar Luminosity, Subdwarf Stars, Symbiotic Stars, Ubv Spectra, Accretion Disks, Astronomical Photometry, Stellar Magnitude

Scientific paper

We present photometric observations of the symbiotic binary AX Per during the ourburst and post-outburst stages. This system contains a hot low mass subdwarf which increases its radius due to thermonuclear burning and fills up its critical surface. A fraction of this material, of the order of 10-5 to 10-4 solar mass/yr is transferred onto the red giant, which is inside its Roche lobe, during the outburst. The observed increase of the star's brightness is caused mainly by collision of impacted matter with the red giant surface. This event causes the wave-like variation of the AX Per light curve during the outburst with an amplitude of 2 mag in the optical UBV region by differing visibility of the collisional emission region in different orbital phases of the binary. UBV light curves during the primary minimum correspond to the total eclipse of the hot component by the cool component. Detailed analysis gives the basic parameters of the binary: Rcool = 102 +/- 3 solar radius, Rhot = 36 +/- 3 solar radius, orbit inclination i = 90 deg +/- 6 deg, luminosities Lhot = 340 (d/2.5 kpc)2 solar luminosity, upper limit of the red giant luminosity Lg = 1800 (d/2.5 kpc)2 solar luminosity, and the luminosity of the wave-like variable light at the maximum Lvmax approximately equal to 1300 (d/2.5 kpc)2 solar luminosity. During the post-outburst period the UBV primary minima indicated a smaller radius and a higher temperature for the hot component. The suggested model disagrees with the accretion disk-powered model for AX Per.

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