X-ray pulsar Comparison Table

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X-ray pulsar comparison table

Subject has orbital period has eccentricity has distance has period has eclipse duration has orbital eccentricity has synonym has definition

Centaurus X-3 2.087 days 5-10 kpc 4.8 s 0.488 days in X-ray e < 0.002 Krzeminski's star A pulsating binary X-ray source in the galactic plane. Optical component is Krzeminski's star, a B0 giant or supergiant. The X-ray component is probably a rotating neutron star of about 0.65-0.83 M_sun. Cen X-3 is speeding up at a rate of about 1 part in 10³-10⁵ per year and will at this rate fall into its companion in about 1000 years.

Hercules X-1 1.7 days e < 0.1 5 kpc 0.24 days (in X-rays) 3U 1653+35 An X-ray pulsar, a member of an occulting binary system. The visible component has been identified as the blue variable HZ Herculis, whose spectrum varies from late A or early F to B. Her X- l has a pulsation period of 1.2378 seconds, presumably its rotation period, and exhibits a 35-day quasi-periodicity in the X-ray region (but not in the optical). It is probably a rotating neutron star in a circular orbit with a mass of about 0.7 M_sun, which is accreting matter from HZ Her. The orbital period is stable, but the pulsation period is speeding up at a rate of about 1 part in 10⁵ per year. The X-ray eclipse lasts 0.24 days.

Subject	has orbital period	has eccentricity	has distance	has period	has eclipse duration	has orbital eccentricity	has synonym	has definition
Centaurus X-3	2.087 days		5-10 kpc	4.8 s	0.488 days in X-ray	e < 0.002	Krzeminski's star	A pulsating binary X-ray source in the galactic plane. Optical component is Krzeminski's star, a B0 giant or supergiant. The X-ray component is probably a rotating neutron star of about 0.65-0.83 M_sun. Cen X-3 is speeding up at a rate of about 1 part in 10³-10⁵ per year and will at this rate fall into its companion in about 1000 years.
Hercules X-1	1.7 days	e < 0.1	5 kpc		0.24 days (in X-rays)		3U 1653+35	An X-ray pulsar, a member of an occulting binary system. The visible component has been identified as the blue variable HZ Herculis, whose spectrum varies from late A or early F to B. Her X- l has a pulsation period of 1.2378 seconds, presumably its rotation period, and exhibits a 35-day quasi-periodicity in the X-ray region (but not in the optical). It is probably a rotating neutron star in a circular orbit with a mass of about 0.7 M_sun, which is accreting matter from HZ Her. The orbital period is stable, but the pulsation period is speeding up at a rate of about 1 part in 10⁵ per year. The X-ray eclipse lasts 0.24 days.

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