Artist's impression of the pulsar surrounded by its bow shock. White rays indicate particles of matter and antimatter being spewed from the star. Its companion star is too close to the pulsar to be visible at this scale.
Depiction of the same pulsar one million times closer showing the effect of its wind on its companion star, which is evaporating. The bow shock is too large to be shown, and at this scale would extend more than 15 miles (24 km) beyond the edge of the computer screen.
astro.wikisort.org - Star
The Black Widow Pulsar (PSR B1957+20) is an eclipsing binary millisecond pulsar in the Milky Way. Discovered in 1988, it is located roughly 6,500 light-years (2,000 parsecs) away from Earth. It orbits with a brown dwarf or Super-Jupiter companion with a period of 9.2 hours with an eclipse duration of approximately 20 minutes. When it was discovered, it was the first such pulsar known.[1] The prevailing theoretical explanation for the system implied that the companion is being destroyed by the strong powerful outflows, or winds, of high-energy particles caused by the neutron star; thus, the sobriquet black widow was applied to the object. Subsequent to this, other objects with similar features have been discovered, and the name has been applied to the class of millisecond pulsars with an ablating companion.
![A visual band light curve for QX Sagittae, adapted from van Paradijs et al. (1988)[2] The light from a nearby star of similar brightness is included, and at the curve's minimum all light comes from that star.](http://upload.wikimedia.org/wikipedia/commons/thumb/f/f1/QXSgeLightCurve.png/220px-QXSgeLightCurve.png)
 The blue and green are optical images of the field in which the black widow pulsar is found, the green indicating the H-alpha bow shock. The red and white are secondary shock structures discovered in x-ray by the Chandra X-ray Observatory. | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Sagitta |
| Right ascension | 19h 59m 36.77s |
| Declination | +20° 48′ 15.12″ |
| Apparent magnitude (V) | 20.4 |
| Details | |
| Rotation | 1.60734 ms |
| Other designations | |
QX Sge, PSR J1959+2048, PSR B1957+20 | |
| Database references | |
| SIMBAD | data |
Later observations of the object showed a bow shock in H-alpha and a smaller-in-extent shock seen in X-rays (as observed by the Chandra X-ray Observatory), indicating a forward velocity of approximately a million kilometers per hour.[3]
In 2010, it was estimated that the neutron star's mass was at least and possibly as high as (the latter of which, if true, would surpass PSR J0740+6620 for the title of most massive neutron star yet detected and place it within range of the Tolman–Oppenheimer–Volkoff limit).[4]
Planets
The pulsar has a substellar companion, possibly a brown dwarf.
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 22 MJ | — | 0.38 | — | — | — |
Gallery
Artist impressions of the Black Widow Pulsar.
See also
References
Wikimedia Commons has media related to Black Widow Pulsars.
- Fruchter, A. S.; Stinebring, D. R.; Taylor, J. H. (May 19, 1988). "A millisecond pulsar in an eclipsing binary". Nature. 333 (6170): 237–9. Bibcode:1988Natur.333..237F. doi:10.1038/333237a0. S2CID 4337525.
- van Paradijs, J.; Allington-Smith, J.; Callanan, P.; Charles, P. A.; Hassall, B. J. M.; Machin, G.; Mason, K. O.; Naylor, T.; Smale, A. P. (August 1988). "Optical observations of the eclipsing binary radio pulsar PSR1957+20". Nature. 334: 684–686. doi:10.1038/334684a0. Retrieved March 5, 2022.
- Chandra Digest (February 27, 2003). "B1957+20: A Cocoon Found Inside the Black Widow's Web". Chandra X-Ray Observatory. Retrieved June 4, 2022.
{{cite web}}: CS1 maint: url-status (link) - Van Kerkwijk, M. H.; Breton, R. P.; Kulkarni, S. R. (2011). "Evidence for a Massive Neutron Star from a Radial-Velocity Study of the Companion to the Black-Widow Pulsar Psr B1957+20". The Astrophysical Journal. 728 (2): 95. arXiv:1009.5427. Bibcode:2011ApJ...728...95V. doi:10.1088/0004-637X/728/2/95. S2CID 37759376.
- "The Extrasolar Planet Encyclopaedia — PSR B1957+20 b". exoplanet.eu. Retrieved January 18, 2021.
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На других языках
[de] Schwarze Witwe (Astronomie)
Eine Schwarze Witwe, engl. Black Widow Pulsar, beschreibt in der Astronomie einen Millisekundenpulsar mit einem massearmen Begleiter in einer engen Umlaufbahn. Die elektromagnetische sowie die Partikelstrahlung des Pulsars erhitzen die Oberfläche seines Begleiters und führen innerhalb einiger Millionen Jahre zur vollständigen Verdampfung des Begleitsterns. Durch die zirkumstellare Materie um den Begleitstern werden die Pulse des Neutronensterns für bis zu 40 % der Bahnumlaufdauer gedämpft. Aufgrund dieses Bedeckungslichtwechsels werden die Schwarzen Witwen auch als Eclipsing Binary Millisecond Pulsars (engl. für bedeckungsveränderliche Millisekundenpulsare in Doppelsternsystemen) bezeichnet.- [en] Black Widow Pulsar
[ru] PSR B1957+20
PSR B1957+20 (Пульсар Чёрная Вдова) — миллисекундный пульсар, является частью двойной системы в созвездии Стрелы. Обнаружен в 1988 году. Является первым обнаруженным пульсаром такого типа[2].Текст в блоке "Читать" взят с сайта "Википедия" и доступен по лицензии Creative Commons Attribution-ShareAlike; в отдельных случаях могут действовать дополнительные условия.
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