To install click the Add extension button. That's it.

The source code for the WIKI 2 extension is being checked by specialists of the Mozilla Foundation, Google, and Apple. You could also do it yourself at any point in time.

4,5
Kelly Slayton
Congratulations on this excellent venture… what a great idea!
Alexander Grigorievskiy
I use WIKI 2 every day and almost forgot how the original Wikipedia looks like.
Live Statistics
English Articles
Improved in 24 Hours
Added in 24 Hours
Languages
Recent
Show all languages
What we do. Every page goes through several hundred of perfecting techniques; in live mode. Quite the same Wikipedia. Just better.
.
Leo
Newton
Brights
Milds

PSR B1259−63/LS 2883

From Wikipedia, the free encyclopedia

LS 2883
Observation data
Epoch J2000      Equinox J2000
Constellation Centaurus
Right ascension 13h 02m 47.655s[1]
Declination −63° 50′ 08.67″[1]
Apparent magnitude (V) 10.34
Characteristics
Spectral type O9.5Ve[2] + pulsar
Astrometry
Proper motion (μ) RA: −6.0[1] mas/yr
Dec.: −5.7[1] mas/yr
Distance7,500[3] ly
Orbit[4]
CompanionSS 2883
Period (P)1237 days
Eccentricity (e)0.87
Inclination (i)36°
Other designations
AAVSO 1256−63, ALS 2883, AX J1302−638, CPD-63° 2495, GSC 08997-01597, Hbg 757, Hen 3-852, INTREF 538, LS 2883, MSX6C G304.1845-00.9916, PSR B1259−63 PSR J1302−6350, THA 17-8, TYC 8997-1597-1, UCAC2 3710789, WRAY 15-1053.[5]
Database references
SIMBADdata
The location of PSR J1302−6350 (circled in red)

PSR J1302−6350 is a pulsar and member of an eclipsing binary star system with the blue O9.5Ve-class star LS 2883. The pair has an eccentric orbit that is inclined to the line of sight from Earth by about 36°, leading to a 40-day-long eclipse each time the pulsar passes behind the star.[4] The pulsar has a period of about 48 ms and a luminosity of 8.3 × 1035 erg/s. It emits very high energy gamma rays that vary on a time scale of several days.[6]

The star LS 2883 has about 10 solar masses and is 6 solar radii in size. The rate of rotation is about 280 km/s at the equator, or 70% of the breakup velocity.[4]

References

  1. ^ a b c d Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27. Bibcode:2000A&A...355L..27H. doi:10.1888/0333750888/2862.
  2. ^ Chernyakova, M.; et al. (March 2014). "Multiwavelength observations of the binary system PSR B1259-63/LS 2883 around the 2010-2011 periastron passage". Monthly Notices of the Royal Astronomical Society. 439 (1): 432–445. arXiv:1401.1386. Bibcode:2014MNRAS.439..432C. doi:10.1093/mnras/stu021. S2CID 55330740.
  3. ^ Universidad de Barcelona (May 2, 2011). "Discovery of Structure of Radio Source from a Pulsar Orbiting a Massive Star". ScienceDaily.
  4. ^ a b c Wang, N.; Johnston, S.; Manchester, R. N. (June 2004). "13 years of timing of PSR B1259-63". Monthly Notices of the Royal Astronomical Society. 351 (2): 599–606. arXiv:astro-ph/0403612. Bibcode:2004MNRAS.351..599W. doi:10.1111/j.1365-2966.2004.07806.x. S2CID 119397388.
  5. ^ "TYC 8997-1597-1 -- Pulsar". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2009-01-06.
  6. ^ Aharonian, F.; et al. (2005). "Discovery of the Binary Pulsar PSR B1259-63 in Very-High-Energy Gamma Rays around Periastron with H.E.S.S.". Astronomy & Astrophysics. 442 (1): 1–10. arXiv:astro-ph/0506280. Bibcode:2005A&A...442....1A. doi:10.1051/0004-6361:20052983. S2CID 11673268.

External links


This page was last edited on 14 May 2023, at 13:08
Basis of this page is in Wikipedia. Text is available under the CC BY-SA 3.0 Unported License. Non-text media are available under their specified licenses. Wikipedia® is a registered trademark of the Wikimedia Foundation, Inc. WIKI 2 is an independent company and has no affiliation with Wikimedia Foundation.