Modeling High-Energy Light Curves of the PSR B1259–63/Ls 2883 Binary Based on 3d SPH Simulations

Takata, Jumpei; Okazaki, Atsuo T.; Nagataki, Shigehiro; Naito, T.; Kawachi, A.; Lee, S.-H.; Mori, M.; Hayasaki, Kimitake; Yamaguchi, Masaki; Owocki, S. P.

doi:10.1088/0004-637x/750/1/70

Cited by 67 publications

(86 citation statements)

References 43 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…For LS 2883, the Be disk should be highly truncated near periastron, both due to the gravitational influence of the pulsar (which is observed in other Be binaries using long baseline optical interferometry; Gies et al 2007) and due to disruption by the pulsar wind ram pressure (predicted by simulations of Okazaki et al 2011;Takata et al 2012). The truncation distance expands rapidly after periastron passage.…”

Section: Evolution Of the Be Star Disk Mass And Size Based On The Hα mentioning

confidence: 96%

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: Evolution Of the Be Star Disk Mass And Size Based On The Hα mentioning

confidence: 96%

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 influence of the circumstellar disk on the nonthermal emission has also been investigated in smooth particle hydrodynamic (SPH) simulations undertaken by Takata et al (2012) which were able to roughly reproduce the X-ray light curve using a very dense disk (∼ 10 −9 g cm −3 ; denser than typical). Here the pre-and post-periastron peaks in the X-ray and TeV light curves were interpreted as the pulsar spin-down power being converted to particle acceleration more efficiently when the pulsar passes through the disk.…”

Section: Introductionmentioning

confidence: 99%

Gamma–Gamma Absorption in the γ-ray Binary System PSR B1259-63/LS 2883

Sushch

Soelen

2017

ApJ

View full text Add to dashboard Cite

The observed TeV light curve from the γ-ray binary PSR B1259-63/LS 2883 shows a decrease in the flux at periastron which has not been fully explained by emission mechanisms alone. This observed decrease can, however, be explained by γγ absorption due to the stellar and disk photons. We calculate the γγ absorption in PSR B1259-63/LS 2883 taking into account photons from both the circumstellar disk and star, assuming the γ rays originate at the position of the pulsar. The γγ absorption due to the circumstellar disk photons produces a ≈ 14% decrease in the flux, and there is a total decrease of ≈ 52% (> 1 TeV) within a few days before periastron, accompanied by a hardening of the γ-ray photon index. While the γγ absorption alone is not sufficient to explain the full complexity of the H.E.S.S. γ-ray light curve it results in a significant decrease in the predicted flux, which is co-incident with the observed decrease. In addition, we have calculated an upper-limit on the γγ absorption, assuming that the emission is produced at the apex of the bow shock. Future observations with CTA during the 2021 periastron passage may be able to confine the location of the emission based on the degree of γγ absorption as well as measure the hardening of the spectrum around periastron.

show abstract

“…Alternatively, the orientation of the cone could deviate from being radially away from the star. The cone has a large opening angle so parts of it are affected by the Be disc (Takata et al 2012). However, this effect is unlikely to persist beyond τ + 60 d and, hence, to significantly impact the lightcurve.…”

Section: Resultsmentioning

confidence: 99%

What caused the GeV flare of PSR B1259-63?

Dubus

Cerutti

2013

A&A

View full text Add to dashboard Cite

Context. PSR B1259-63 is a gamma-ray binary system composed of a high spindown pulsar and a massive star. Non-thermal emission up to TeV energies is observed near periastron passage, attributed to emission from high energy e + e − pairs accelerated at the shock with the circumstellar material from the companion star, resulting in a small-scale pulsar wind nebula. Weak gamma-ray emission was detected by the Fermi/LAT at the last periastron passage, unexpectedly followed 30 days later by a strong flare, limited to the GeV band, during which the luminosity nearly reached the spindown power of the pulsar. The origin of this GeV flare remains mysterious. Aims. We investigate whether the flare could have been caused by pairs, located in the vicinity of the pulsar, up-scattering X-ray photons from the surrounding pulsar wind nebula rather than UV stellar photons, as usually assumed. Such a model is suggested by the geometry of the interaction region at the time of the flare. Methods. We compute the gamma-ray lightcurve for this scenario, based on a simplified description of the interaction region, and compare it to the observations. Results. The GeV lightcurve peaks well after periastron with this geometry. The pairs are inferred to have a Lorentz factor ≈500. They also produce an MeV flare with a luminosity ≈10 34 erg s −1 prior to periastron passage. A significant drawback is the very high energy density of target photons required for efficient GeV emission. Conclusions. We propose to associate the GeV-emitting pairs with the Maxwellian expected at shock locations corresponding to high pulsar latitudes, while the rest of the non-thermal emission arises from pairs accelerated in the equatorial region of the pulsar wind termination shock.

show abstract

Modeling High-Energy Light Curves of the PSR B1259–63/Ls 2883 Binary Based on 3d SPH Simulations

Cited by 67 publications

References 43 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

Gamma–Gamma Absorption in the γ-ray Binary System PSR B1259-63/LS 2883

What caused the GeV flare of PSR B1259-63?

Contact Info

Product

Resources

About