Delayed hard photons from gamma-ray bursts

J. I. Katz

doi:10.1086/187503

Delayed hard photons from gamma-ray bursts

J. I. Katz

Department of Physics

Research output: Contribution to journal › Article › peer-review

58 Scopus citations

Abstract

The delayed hard (up to 25 GeV) photons observed more than an hour following a gamma-ray burst on 1994 February 17 may result from the collisions of relativistic nucleons with a dense cloud, producing π⁰. The required cloud density is ∼2 × 10¹¹ cm^-3. This cloud may be the remains of the disrupted envelope of a neutron star, and may survive as an excretion disk of ∼10¹⁴-10¹⁵ cm radius around the coalescing binary.

Original language	English
Pages (from-to)	L27-L29
Journal	Astrophysical Journal
Volume	432
Issue number	1 PART 2
DOIs	https://doi.org/10.1086/187503
State	Published - Sep 1 1994

Keywords

Gamma rays: bursts
Stars: neutron

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10.1086/187503

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title = "Delayed hard photons from gamma-ray bursts",

abstract = "The delayed hard (up to 25 GeV) photons observed more than an hour following a gamma-ray burst on 1994 February 17 may result from the collisions of relativistic nucleons with a dense cloud, producing π0. The required cloud density is ∼2 × 1011 cm-3. This cloud may be the remains of the disrupted envelope of a neutron star, and may survive as an excretion disk of ∼1014-1015 cm radius around the coalescing binary.",

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doi = "10.1086/187503",

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N2 - The delayed hard (up to 25 GeV) photons observed more than an hour following a gamma-ray burst on 1994 February 17 may result from the collisions of relativistic nucleons with a dense cloud, producing π0. The required cloud density is ∼2 × 1011 cm-3. This cloud may be the remains of the disrupted envelope of a neutron star, and may survive as an excretion disk of ∼1014-1015 cm radius around the coalescing binary.

AB - The delayed hard (up to 25 GeV) photons observed more than an hour following a gamma-ray burst on 1994 February 17 may result from the collisions of relativistic nucleons with a dense cloud, producing π0. The required cloud density is ∼2 × 1011 cm-3. This cloud may be the remains of the disrupted envelope of a neutron star, and may survive as an excretion disk of ∼1014-1015 cm radius around the coalescing binary.

KW - Gamma rays: bursts

KW - Stars: neutron

UR - https://www.scopus.com/pages/publications/12044249192

U2 - 10.1086/187503

DO - 10.1086/187503

M3 - Article

AN - SCOPUS:12044249192

SN - 0004-637X

VL - 432

SP - L27-L29

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1 PART 2

ER -

Delayed hard photons from gamma-ray bursts

Abstract

Keywords

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