High-energy emission from the double pulsar system J0737-3039

Jonathan Granot; Peter Mészáros

doi:10.1086/422637

High-energy emission from the double pulsar system J0737-3039

Research output: Contribution to journal › Review article › peer-review

Abstract

We discuss the effects of particle acceleration at the bow shocks expected in the binary pulsar system J0737-3039, because of the wind from pulsar A interacting with both the interstellar medium (ISM) and the magnetosphere of pulsar B. In this model, we find that the likeliest source for the X-rays observed by Chandra is the emission from the shocked wind of pulsar A as it interacts with the ISM. In this case, for favorable model parameter values, better statistics might help Chandra marginally resolve the source. A consequence of the model is a power-law high-energy spectrum extending up to ≲60 keV, at a level of ∼2 × 10^-13 ergs cm ^-2s^-1.

Original language	English
Pages (from-to)	L17-L20
Journal	Astrophysical Journal
Volume	609
Issue number	1 II
DOIs	https://doi.org/10.1086/422637
State	Published - 1 Jul 2004
Externally published	Yes

Keywords

Gamma rays: observations
Pulsars: general
Pulsars: individual (PSR 0737-3039A, PSR 0737-3039B)
Radiation mechanisms: nonthermal
X-rays: binaries

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10.1086/422637

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title = "High-energy emission from the double pulsar system J0737-3039",

abstract = "We discuss the effects of particle acceleration at the bow shocks expected in the binary pulsar system J0737-3039, because of the wind from pulsar A interacting with both the interstellar medium (ISM) and the magnetosphere of pulsar B. In this model, we find that the likeliest source for the X-rays observed by Chandra is the emission from the shocked wind of pulsar A as it interacts with the ISM. In this case, for favorable model parameter values, better statistics might help Chandra marginally resolve the source. A consequence of the model is a power-law high-energy spectrum extending up to ≲60 keV, at a level of ∼2 × 10-13 ergs cm -2s-1.",

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T1 - High-energy emission from the double pulsar system J0737-3039

AU - Granot, Jonathan

AU - Mészáros, Peter

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N2 - We discuss the effects of particle acceleration at the bow shocks expected in the binary pulsar system J0737-3039, because of the wind from pulsar A interacting with both the interstellar medium (ISM) and the magnetosphere of pulsar B. In this model, we find that the likeliest source for the X-rays observed by Chandra is the emission from the shocked wind of pulsar A as it interacts with the ISM. In this case, for favorable model parameter values, better statistics might help Chandra marginally resolve the source. A consequence of the model is a power-law high-energy spectrum extending up to ≲60 keV, at a level of ∼2 × 10-13 ergs cm -2s-1.

AB - We discuss the effects of particle acceleration at the bow shocks expected in the binary pulsar system J0737-3039, because of the wind from pulsar A interacting with both the interstellar medium (ISM) and the magnetosphere of pulsar B. In this model, we find that the likeliest source for the X-rays observed by Chandra is the emission from the shocked wind of pulsar A as it interacts with the ISM. In this case, for favorable model parameter values, better statistics might help Chandra marginally resolve the source. A consequence of the model is a power-law high-energy spectrum extending up to ≲60 keV, at a level of ∼2 × 10-13 ergs cm -2s-1.

KW - Gamma rays: observations

KW - Pulsars: general

KW - Pulsars: individual (PSR 0737-3039A, PSR 0737-3039B)

KW - Radiation mechanisms: nonthermal

KW - X-rays: binaries

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High-energy emission from the double pulsar system J0737-3039

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