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Article: Gamma-ray emission properties from mature pulsars in the Galaxy and in the Gould Belt
Title | Gamma-ray emission properties from mature pulsars in the Galaxy and in the Gould Belt |
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Authors | |
Keywords | Gamma rays: theory Pulsars: general Stars: neutron Stars: statistics |
Issue Date | 2004 |
Publisher | Institute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205 |
Citation | Astrophysical Journal Letters, 2004, v. 608 n. 1 I, p. 418-426 How to Cite? |
Abstract | We study the γ-ray emission properties of pulsars by using a new self-consistent outer gap model. The outer gap can exist in pulsars older than 1 million yr if the effect of magnetic inclination angle, as well as the average properties of the outer gap, are considered. The mature γ-ray pulsars, whose ages are between 0.3 and 3 million yr, are able to move up to high Galactic latitude. Moreover, their γ-ray luminosities are weaker, and their spectra are significantly softer than those of younger γ-ray pulsars in the Galactic plane. We use a Monte Carlo method to simulate the statistical properties of γ-ray pulsars in the Galaxy as well as in the Gould Belt. We find that γ-ray pulsars located at |b| < 5° and |b| > 5° have very different properties. High Galactic latitude γ-ray pulsars are dominated by mature pulsars with longer periods, weaker fluxes, and softer spectra. If the pulsar birth rates in the Galaxy and the Gould Belt are ∼10 -2 and ∼2 × 10 -5 yr -1, respectively, there are 42 and 35 radio-quiet γ-ray pulsars for |b| < 5° and |b| > 5°, respectively. The number of radio-quiet γ-ray pulsars from the Gould Belt are 2 and 13 for |b| < 5° and |b| > 5°, respectively. We suggest that a good fraction of unidentified EGRET γ-ray sources may be these radio-quiet γ-ray pulsars. Furthermore, γ-ray pulsars located at |b| > 5° satisfy L γ α L sd β, whereas L γ α L sd δ for γ-ray pulsars in the Galactic plane, where β ∼ 0.6 and δ ∼ 0.3, respectively. |
Persistent Identifier | http://hdl.handle.net/10722/43447 |
ISSN | 2023 Impact Factor: 8.8 2023 SCImago Journal Rankings: 2.766 |
ISI Accession Number ID | |
References |
DC Field | Value | Language |
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dc.contributor.author | Cheng, KS | en_HK |
dc.contributor.author | Zhang, L | en_HK |
dc.contributor.author | Leung, P | en_HK |
dc.contributor.author | Jiang, ZJ | en_HK |
dc.date.accessioned | 2007-03-23T04:45:52Z | - |
dc.date.available | 2007-03-23T04:45:52Z | - |
dc.date.issued | 2004 | en_HK |
dc.identifier.citation | Astrophysical Journal Letters, 2004, v. 608 n. 1 I, p. 418-426 | en_HK |
dc.identifier.issn | 2041-8205 | en_HK |
dc.identifier.uri | http://hdl.handle.net/10722/43447 | - |
dc.description.abstract | We study the γ-ray emission properties of pulsars by using a new self-consistent outer gap model. The outer gap can exist in pulsars older than 1 million yr if the effect of magnetic inclination angle, as well as the average properties of the outer gap, are considered. The mature γ-ray pulsars, whose ages are between 0.3 and 3 million yr, are able to move up to high Galactic latitude. Moreover, their γ-ray luminosities are weaker, and their spectra are significantly softer than those of younger γ-ray pulsars in the Galactic plane. We use a Monte Carlo method to simulate the statistical properties of γ-ray pulsars in the Galaxy as well as in the Gould Belt. We find that γ-ray pulsars located at |b| < 5° and |b| > 5° have very different properties. High Galactic latitude γ-ray pulsars are dominated by mature pulsars with longer periods, weaker fluxes, and softer spectra. If the pulsar birth rates in the Galaxy and the Gould Belt are ∼10 -2 and ∼2 × 10 -5 yr -1, respectively, there are 42 and 35 radio-quiet γ-ray pulsars for |b| < 5° and |b| > 5°, respectively. The number of radio-quiet γ-ray pulsars from the Gould Belt are 2 and 13 for |b| < 5° and |b| > 5°, respectively. We suggest that a good fraction of unidentified EGRET γ-ray sources may be these radio-quiet γ-ray pulsars. Furthermore, γ-ray pulsars located at |b| > 5° satisfy L γ α L sd β, whereas L γ α L sd δ for γ-ray pulsars in the Galactic plane, where β ∼ 0.6 and δ ∼ 0.3, respectively. | en_HK |
dc.format.extent | 560130 bytes | - |
dc.format.extent | 12158 bytes | - |
dc.format.mimetype | application/pdf | - |
dc.format.mimetype | text/plain | - |
dc.language | eng | en_HK |
dc.publisher | Institute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205 | en_HK |
dc.relation.ispartof | Astrophysical Journal Letters | en_HK |
dc.rights | The Astrophysical Journal. Copyright © University of Chicago Press. | en_HK |
dc.subject | Gamma rays: theory | en_HK |
dc.subject | Pulsars: general | en_HK |
dc.subject | Stars: neutron | en_HK |
dc.subject | Stars: statistics | en_HK |
dc.title | Gamma-ray emission properties from mature pulsars in the Galaxy and in the Gould Belt | en_HK |
dc.type | Article | en_HK |
dc.identifier.openurl | http://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0004-637X&volume=608&issue=1 pt 1&spage=418&epage=426&date=2004&atitle=Gamma-Ray+Emission+Properties+from+Mature+Pulsars+in+the+Galaxy+and+in+the+Gould+Belt | en_HK |
dc.identifier.email | Cheng, KS: hrspksc@hkucc.hku.hk | en_HK |
dc.identifier.authority | Cheng, KS=rp00675 | en_HK |
dc.description.nature | published_or_final_version | en_HK |
dc.identifier.doi | 10.1086/386537 | en_HK |
dc.identifier.scopus | eid_2-s2.0-3142710943 | en_HK |
dc.identifier.hkuros | 97119 | - |
dc.relation.references | http://www.scopus.com/mlt/select.url?eid=2-s2.0-3142710943&selection=ref&src=s&origin=recordpage | en_HK |
dc.identifier.volume | 608 | en_HK |
dc.identifier.issue | 1 I | en_HK |
dc.identifier.spage | 418 | en_HK |
dc.identifier.epage | 426 | en_HK |
dc.identifier.isi | WOS:000221881200036 | - |
dc.publisher.place | United Kingdom | en_HK |
dc.identifier.scopusauthorid | Cheng, KS=9745798500 | en_HK |
dc.identifier.scopusauthorid | Zhang, L=38762428100 | en_HK |
dc.identifier.scopusauthorid | Leung, P=7401749062 | en_HK |
dc.identifier.scopusauthorid | Jiang, ZJ=7404280278 | en_HK |
dc.identifier.issnl | 2041-8205 | - |