PSR 1259-63 - A binary radio pulsar with a Be star companion

Johnston, S.; Manchester, R. N.; Lyne, A. G.; Bailes, M.; Kaspi, V. M.; Qiao, G. J.; D’Amico, N.

doi:10.1086/186300

Cited by 367 publications

(349 citation statements)

References 0 publications

Supporting

Mentioning

346

Contrasting

Order By: Relevance

“…The binary system PSR B1259−63 is comprised of a 47.76 ms radio pulsar in a highly eccentric orbit (e ≈ 0.87, P ≈ 3.4 years) around the massive main sequence O9.5Ve star LS 2883 (Johnston et al 1992; Negueruela et al 2011). The companion shows evidence for an equatorial disk in its optical spectrum, and it has generally been classified as a Be star.…”

Section: Introductionmentioning

confidence: 99%

Multi-wavelength observations of the binary system PSR B1259−63/LS 2883 around the 2014 periastron passage

Chernyakova

Neronov

Soelen

et al. 2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We report on broad multi-wavelength observations of the 2010-2011 periastron passage of the γ-ray loud binary system PSR B1259−63. High resolution interferometric radio observations establish extended radio emission trailing the position of the pulsar. Observations with the Fermi Gamma-ray Space Telescope reveal GeV γ-ray flaring activity of the system, reaching the spin-down luminosity of the pulsar, around 30 days after periastron. There are no clear signatures of variability at radio, X-ray and TeV energies at the time of the GeV flare. Variability around periastron in the Hα emission line, can be interpreted as the gravitational interaction between the pulsar and the circumstellar disk. The equivalent width of the Hα grows from a few days before periastron until a few days later, and decreases again between 18 and 46 days after periastron. In near infrared we observe the similar decrease of the equivalent width of Brγ line between the 40th and 117th day after the periastron. For the idealized disk, the variability of the Hα line represents the variability of the mass and size of the disk. We discuss possible physical relations between the state of the disk and GeV emission under assumption that GeV flare is directly related to the decrease of the disk size.

show abstract

Section: Introductionmentioning

confidence: 99%

Multi-wavelength observations of the binary system PSR B1259−63/LS 2883 around the 2014 periastron passage

Chernyakova

Neronov

Soelen

et al. 2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

show abstract

“…The history of the Scenario Machine can be briefly summarized as follows: a+e - Kornilov & Lipunov (1983a), Kornilov & Lipunov (1983b) Massive binaries a+e +f - Kornilov & Lipunov (1984) Massive binaries a+b + c+d+e - Lipunov & Postnov (1987b) Low Massive Binaries a + d - Dewey & Cordes (1987) Massive Binaries + radiopulsar evolution a+b+c+d+e+f -Scenario Machine Lipunov & Postnov (1987a), Lipunov & Postnov (1987b), Lipunov & Postnov (1988) The results obtained with the Scenario Machine include the following: 1) Prediction of nearly 100 new stages of binary systems with magnetized compact companions; 2) Prediction of millisecond X-ray accreting pulsars (see Kornilov & Lipunov (1983b)), later confirmed by discovery of A0538-66 (P = 0.067 s); 3)Explanation of some of the ultrasoft superluminous sources as superaccreting compact stars in binaries (Lipunov et al (1993)), which was confirmed by the discovery of a transient X-ray pulsar RX J0059.2-7138 in the Small Magellanic Cloud (SMC) (Hughes (1994)); 4) Prediction of the strong dependence of the X-ray luminosity on star formation history in galaxies; 5) Prediction and estimation of the number of binary radiopulsars with OB-stars (1 per 700 visible galactic pulsars) (Kornilov & Lipunov (1984), ), which was confirmed by discovery of PSR B1259-63 (Johnston et al (1992)); 6) Estimation of the number of binary radiopulsars with black holes (Lipunov (1994)); 7) Calculation of the gravitational wave background formed by galactic and extragalactic binaries (Lipunov & Postnov (1987a), Lipunov & Postnov (1988); Lipunov et al (1995a)); 8) Anisotropy of supernova explosions giving "kick"-velocities of young pulsars of 70-100 km/s (Kornilov & Lipunov (1984); similar estimates are given by Dewey & Cordes (1987)), a more detailed discussion will be given below; 9) A significant evolution of Xray luminosity of the galaxies (discovered on RXTE, Chandra, INTEGRAL) as indicator of star formation rate history (Tatarintzeva et al (1989)); 10) A significant evolution of supernova rates and binary NS merging rates at cosmological distances (Lipunov & Postnov (1988); Lipunov et al (1995b)). …”

Section: Introductionmentioning

confidence: 88%

Population synthesis of binary relativistic stars

Липунов

2005

Proc. IAU

View full text Add to dashboard Cite

show abstract

“…The system is located at a distance of 2.3 kpc. It is the only gamma-ray binary system for which the nature of the compact object is known [3,4].…”

Section: Observations Of Psr B1259-63/ls 2883mentioning

confidence: 99%

Observations of binary systems with the H.E.S.S. telescopes

2017

AIP Conference Proceedings

View full text Add to dashboard Cite

Abstract. Observations of binary systems obtained recently with the High Energy Stereoscopic System (H.E.S.S) of Cherenkov telescopes are reported. The outcomes of a detailed observation campaign on PSR B1259-63 during its periastron passage in 2014 will be presented. This system was observed for the first time with H.E.S.S. II, providing spectra and light curves down to 200 GeV, which will be compared with observations conducted during previous periastron passages and with results from an analysis of contemporaneously taken Fermi-LAT data. Also long-term observations of LS 5039 with H.E.S.S in phase I and phase II are reported. This source was monitored at very high energies (VHEs) in a period of time spanning more than ten years. Its spectral energy distribution measured with H.E.S.S. II extends down to 120 GeV. Spectral results from the Fermi-LAT observations are shown as well, and the compatibility with H.E.S.S. results in the overlapping energy range is discussed. The identification of the new gamma-ray binary candidate HESS J1832-093 will also be presented. Furthermore, the search for VHE emission from the microquasars GRS 1915+105, Circinus X-1 and V4641 Sgr based on data from H.E.S.S. observations conducted contemporaneously with the RXTE satellite experiment will be reported. These data provide constraints on the integral gamma-ray flux at different X-ray states of the three sources.

show abstract

PSR 1259-63 - A binary radio pulsar with a Be star companion

Cited by 367 publications

References 0 publications

Multi-wavelength observations of the binary system PSR B1259−63/LS 2883 around the 2014 periastron passage

Multi-wavelength observations of the binary system PSR B1259−63/LS 2883 around the 2014 periastron passage

Population synthesis of binary relativistic stars

Observations of binary systems with the H.E.S.S. telescopes

Contact Info

Product

Resources

About