DQ Herculis Comparison Table

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physical object > natural object > celestial body > collection of stars > star system > binary star > close binary > eclipsing binary > DQ Herculis

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DQ Herculis comparison table

Subject has energy release become has orbital period is an instance of has erruption date has acronym has primary star has secondary star is a kind of has use has synonym has definition

eclipsing binary close binary Eclipsing variables whose orbital plane lies so nearly in the line of sight that eclipses, as seen from the Earth, can occur and can be detected from their light curves.

slow nova 10⁴⁴ ergs naked eye star CV nova nova peak brightness distance determination explosive variable A nova whose light curve shows a much more gradual development - i.e., rise time of several days, maximum of several weeks, slower decline, amplitude only about 10 mag.

DQ Herculis 10⁴⁴ ergs naked eye star 4^h39^m eclipsing binary 1934 CV white dwarf M dwarf nova peak brightness distance determination Nova Herculis 1934 A slow nova which also happens to be an eclipsing binary. It also has a regular flickering period of 71 seconds, the shortest period of regular variations known, except for pulsars and compact X-ray objects. It is probably composed of an M dwarf and a white dwarf with an accretion disk.

Subject	has energy release	become	has orbital period	is an instance of	has erruption date	has acronym	has primary star	has secondary star	is a kind of	has use	has synonym	has definition
eclipsing binary									close binary			Eclipsing variables whose orbital plane lies so nearly in the line of sight that eclipses, as seen from the Earth, can occur and can be detected from their light curves.
slow nova	10⁴⁴ ergs	naked eye star				CV			nova	nova peak brightness distance determination	explosive variable	A nova whose light curve shows a much more gradual development - i.e., rise time of several days, maximum of several weeks, slower decline, amplitude only about 10 mag.
DQ Herculis	10⁴⁴ ergs	naked eye star	4^h39^m	eclipsing binary	1934	CV	white dwarf	M dwarf		nova peak brightness distance determination	Nova Herculis 1934	A slow nova which also happens to be an eclipsing binary. It also has a regular flickering period of 71 seconds, the shortest period of regular variations known, except for pulsars and compact X-ray objects. It is probably composed of an M dwarf and a white dwarf with an accretion disk.

Next eclipsing binary: epsilon Aurigae Up: eclipsing binary, slow nova Previous eclipsing binary: CV Serpentis