The photometric periods of the intermediate polar EX Hydrae

Details The photometric periods of the intermediate polar EX Hydrae The photometric periods of the intermediate polar EX Hydrae

Nov 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...225...97s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 225, no. 1, Nov. 1989, p. 97-104.

Astronomy and Astrophysics

Astrophysics

17

Astronomical Photometry, Cataclysmic Variables, Eclipsing Binary Stars, White Dwarf Stars, Light Curve, Periodic Variations

Scientific paper

Five-color photometry of the dwarf nova EX Hya during its quiescent state revealed that no independent modulations of the optical light are persistent other than the 98-min binary orbital period and the 67-min spin period of the white dwarf. No indication could be found for additional photometric periods claimed previously, in particular, a possible period of 46.2 min. However, a transient modulation with P = 28.4 min was observed which may be explained as a beat of the 67-min period and half the orbital period, and which gives some evidence that a significant orbital-phase-dependent amplitude modulation of the 67-min variation may occur in EX Hya. The observations confirm that the center of the optical eclipse wanders back and forth in time by + or - 20 s as a function of 67-min phase, suggesting that the eclipsed optical source is locked to the white dwarf and centered at a radial distance of about 1.5 x 10 to the 9th cm. The U-B color variation supports the presence of a Balmer emission component which shows a more pronounced 67-min modulation than the remainder of the light and which is less strongly eclipsed.

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