An estimate of the system parameters in the dwarf nova IP Peg

Details An estimate of the system parameters in the dwarf nova IP Peg An estimate of the system parameters in the dwarf nova IP Peg

Oct 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986mnras.222..645w&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 222, Oct. 1, 1986, p. 645-654.

Astronomy and Astrophysics

Astronomy

52

Dwarf Novae, Eclipsing Binary Stars, Stellar Mass, Stellar Spectrophotometry, Stellar Structure, Boundary Layers, Orbital Elements, Stellar Evolution, White Dwarf Stars

Scientific paper

High-speed photometry of the eclipsing dwarf nova IP Peg is used to estimate the geometry of the binary system and the masses of its components. The white dwarf is surrounded by an extended boundary layer and has a mass of at least 0.3 solar mass, probably much greater, depending on the thickness of the boundary layer and the orbital inclination. Its mass could be as high as 0.9 solar mass for an inclination of 80.9 deg. The mass of the secondary star is greater than 0.09 solar mass, probably a lot higher. IP Peg could be earlier in the evolutionary sequence of dwarf novae than the ultra-short-period systems (P less than 2 hr).

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