Gamma-ray bursts from galactic neutron stars?
The γ-ray burst distance scale is not known and quiescent counterparts of γ-ray bursts have not been unambiguously identified in any wavelength band. It is generally assumed that γ-ray bursts originate on or near neutron stars in the general vicinity of our galaxy. Statistical tools for determining...
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| Autor*in: |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
1989 |
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| Reproduktion: |
Elsevier Journal Backfiles on ScienceDirect 1907 - 2002 |
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| Übergeordnetes Werk: |
in: Nuclear Physics B (Proceedings Supplements) - Amsterdam : Elsevier, 10(1989), 2, Seite 27-37 |
| Übergeordnetes Werk: |
volume:10 ; year:1989 ; number:2 ; pages:27-37 |
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| 520 | |a The γ-ray burst distance scale is not known and quiescent counterparts of γ-ray bursts have not been unambiguously identified in any wavelength band. It is generally assumed that γ-ray bursts originate on or near neutron stars in the general vicinity of our galaxy. Statistical tools for determining the γ-ray burst spatial distribution are their brightness distribution (''log N - log S'' and V/V"m"a"x) and their angular distribution on the celestial sphere. We discuss in detail the dipole- and quadrupole moments and the angular autocovariance function ω(θ) of the positional data. The observations suggest zero angular correlation and small multipole moments which places severe constraints on the spatial distribution of γ-ray bursts. We discuss a Monte Carlo simulation of the population of galactic neutron stars which can be used to test the hypothesis that γ-ray bursts originate on galactic neutron stars. | ||
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(DE-627)NLEJ181736314 (DE-599)GBVNLZ181736314 DE-627 ger DE-627 rakwb eng Gamma-ray bursts from galactic neutron stars? 1989 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier The γ-ray burst distance scale is not known and quiescent counterparts of γ-ray bursts have not been unambiguously identified in any wavelength band. It is generally assumed that γ-ray bursts originate on or near neutron stars in the general vicinity of our galaxy. Statistical tools for determining the γ-ray burst spatial distribution are their brightness distribution (''log N - log S'' and V/V"m"a"x) and their angular distribution on the celestial sphere. We discuss in detail the dipole- and quadrupole moments and the angular autocovariance function ω(θ) of the positional data. The observations suggest zero angular correlation and small multipole moments which places severe constraints on the spatial distribution of γ-ray bursts. We discuss a Monte Carlo simulation of the population of galactic neutron stars which can be used to test the hypothesis that γ-ray bursts originate on galactic neutron stars. Elsevier Journal Backfiles on ScienceDirect 1907 - 2002 Hartmann, D. oth Epstein, R.I. oth Woosley, S.E. oth in Nuclear Physics B (Proceedings Supplements) Amsterdam : Elsevier 10(1989), 2, Seite 27-37 (DE-627)NLEJ181551780 (DE-600)1466572-4 0920-5632 nnns volume:10 year:1989 number:2 pages:27-37 http://dx.doi.org/10.1016/0920-5632(89)90035-2 GBV_USEFLAG_H ZDB-1-SDJ GBV_NL_ARTICLE AR 10 1989 2 27-37 |
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(DE-627)NLEJ181736314 (DE-599)GBVNLZ181736314 DE-627 ger DE-627 rakwb eng Gamma-ray bursts from galactic neutron stars? 1989 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier The γ-ray burst distance scale is not known and quiescent counterparts of γ-ray bursts have not been unambiguously identified in any wavelength band. It is generally assumed that γ-ray bursts originate on or near neutron stars in the general vicinity of our galaxy. Statistical tools for determining the γ-ray burst spatial distribution are their brightness distribution (''log N - log S'' and V/V"m"a"x) and their angular distribution on the celestial sphere. We discuss in detail the dipole- and quadrupole moments and the angular autocovariance function ω(θ) of the positional data. The observations suggest zero angular correlation and small multipole moments which places severe constraints on the spatial distribution of γ-ray bursts. We discuss a Monte Carlo simulation of the population of galactic neutron stars which can be used to test the hypothesis that γ-ray bursts originate on galactic neutron stars. Elsevier Journal Backfiles on ScienceDirect 1907 - 2002 Hartmann, D. oth Epstein, R.I. oth Woosley, S.E. oth in Nuclear Physics B (Proceedings Supplements) Amsterdam : Elsevier 10(1989), 2, Seite 27-37 (DE-627)NLEJ181551780 (DE-600)1466572-4 0920-5632 nnns volume:10 year:1989 number:2 pages:27-37 http://dx.doi.org/10.1016/0920-5632(89)90035-2 GBV_USEFLAG_H ZDB-1-SDJ GBV_NL_ARTICLE AR 10 1989 2 27-37 |
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(DE-627)NLEJ181736314 (DE-599)GBVNLZ181736314 DE-627 ger DE-627 rakwb eng Gamma-ray bursts from galactic neutron stars? 1989 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier The γ-ray burst distance scale is not known and quiescent counterparts of γ-ray bursts have not been unambiguously identified in any wavelength band. It is generally assumed that γ-ray bursts originate on or near neutron stars in the general vicinity of our galaxy. Statistical tools for determining the γ-ray burst spatial distribution are their brightness distribution (''log N - log S'' and V/V"m"a"x) and their angular distribution on the celestial sphere. We discuss in detail the dipole- and quadrupole moments and the angular autocovariance function ω(θ) of the positional data. The observations suggest zero angular correlation and small multipole moments which places severe constraints on the spatial distribution of γ-ray bursts. We discuss a Monte Carlo simulation of the population of galactic neutron stars which can be used to test the hypothesis that γ-ray bursts originate on galactic neutron stars. Elsevier Journal Backfiles on ScienceDirect 1907 - 2002 Hartmann, D. oth Epstein, R.I. oth Woosley, S.E. oth in Nuclear Physics B (Proceedings Supplements) Amsterdam : Elsevier 10(1989), 2, Seite 27-37 (DE-627)NLEJ181551780 (DE-600)1466572-4 0920-5632 nnns volume:10 year:1989 number:2 pages:27-37 http://dx.doi.org/10.1016/0920-5632(89)90035-2 GBV_USEFLAG_H ZDB-1-SDJ GBV_NL_ARTICLE AR 10 1989 2 27-37 |
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(DE-627)NLEJ181736314 (DE-599)GBVNLZ181736314 DE-627 ger DE-627 rakwb eng Gamma-ray bursts from galactic neutron stars? 1989 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier The γ-ray burst distance scale is not known and quiescent counterparts of γ-ray bursts have not been unambiguously identified in any wavelength band. It is generally assumed that γ-ray bursts originate on or near neutron stars in the general vicinity of our galaxy. Statistical tools for determining the γ-ray burst spatial distribution are their brightness distribution (''log N - log S'' and V/V"m"a"x) and their angular distribution on the celestial sphere. We discuss in detail the dipole- and quadrupole moments and the angular autocovariance function ω(θ) of the positional data. The observations suggest zero angular correlation and small multipole moments which places severe constraints on the spatial distribution of γ-ray bursts. We discuss a Monte Carlo simulation of the population of galactic neutron stars which can be used to test the hypothesis that γ-ray bursts originate on galactic neutron stars. Elsevier Journal Backfiles on ScienceDirect 1907 - 2002 Hartmann, D. oth Epstein, R.I. oth Woosley, S.E. oth in Nuclear Physics B (Proceedings Supplements) Amsterdam : Elsevier 10(1989), 2, Seite 27-37 (DE-627)NLEJ181551780 (DE-600)1466572-4 0920-5632 nnns volume:10 year:1989 number:2 pages:27-37 http://dx.doi.org/10.1016/0920-5632(89)90035-2 GBV_USEFLAG_H ZDB-1-SDJ GBV_NL_ARTICLE AR 10 1989 2 27-37 |
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(DE-627)NLEJ181736314 (DE-599)GBVNLZ181736314 DE-627 ger DE-627 rakwb eng Gamma-ray bursts from galactic neutron stars? 1989 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier The γ-ray burst distance scale is not known and quiescent counterparts of γ-ray bursts have not been unambiguously identified in any wavelength band. It is generally assumed that γ-ray bursts originate on or near neutron stars in the general vicinity of our galaxy. Statistical tools for determining the γ-ray burst spatial distribution are their brightness distribution (''log N - log S'' and V/V"m"a"x) and their angular distribution on the celestial sphere. We discuss in detail the dipole- and quadrupole moments and the angular autocovariance function ω(θ) of the positional data. The observations suggest zero angular correlation and small multipole moments which places severe constraints on the spatial distribution of γ-ray bursts. We discuss a Monte Carlo simulation of the population of galactic neutron stars which can be used to test the hypothesis that γ-ray bursts originate on galactic neutron stars. Elsevier Journal Backfiles on ScienceDirect 1907 - 2002 Hartmann, D. oth Epstein, R.I. oth Woosley, S.E. oth in Nuclear Physics B (Proceedings Supplements) Amsterdam : Elsevier 10(1989), 2, Seite 27-37 (DE-627)NLEJ181551780 (DE-600)1466572-4 0920-5632 nnns volume:10 year:1989 number:2 pages:27-37 http://dx.doi.org/10.1016/0920-5632(89)90035-2 GBV_USEFLAG_H ZDB-1-SDJ GBV_NL_ARTICLE AR 10 1989 2 27-37 |
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The γ-ray burst distance scale is not known and quiescent counterparts of γ-ray bursts have not been unambiguously identified in any wavelength band. It is generally assumed that γ-ray bursts originate on or near neutron stars in the general vicinity of our galaxy. Statistical tools for determining the γ-ray burst spatial distribution are their brightness distribution (''log N - log S'' and V/V"m"a"x) and their angular distribution on the celestial sphere. We discuss in detail the dipole- and quadrupole moments and the angular autocovariance function ω(θ) of the positional data. The observations suggest zero angular correlation and small multipole moments which places severe constraints on the spatial distribution of γ-ray bursts. We discuss a Monte Carlo simulation of the population of galactic neutron stars which can be used to test the hypothesis that γ-ray bursts originate on galactic neutron stars. |
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The γ-ray burst distance scale is not known and quiescent counterparts of γ-ray bursts have not been unambiguously identified in any wavelength band. It is generally assumed that γ-ray bursts originate on or near neutron stars in the general vicinity of our galaxy. Statistical tools for determining the γ-ray burst spatial distribution are their brightness distribution (''log N - log S'' and V/V"m"a"x) and their angular distribution on the celestial sphere. We discuss in detail the dipole- and quadrupole moments and the angular autocovariance function ω(θ) of the positional data. The observations suggest zero angular correlation and small multipole moments which places severe constraints on the spatial distribution of γ-ray bursts. We discuss a Monte Carlo simulation of the population of galactic neutron stars which can be used to test the hypothesis that γ-ray bursts originate on galactic neutron stars. |
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The γ-ray burst distance scale is not known and quiescent counterparts of γ-ray bursts have not been unambiguously identified in any wavelength band. It is generally assumed that γ-ray bursts originate on or near neutron stars in the general vicinity of our galaxy. Statistical tools for determining the γ-ray burst spatial distribution are their brightness distribution (''log N - log S'' and V/V"m"a"x) and their angular distribution on the celestial sphere. We discuss in detail the dipole- and quadrupole moments and the angular autocovariance function ω(θ) of the positional data. The observations suggest zero angular correlation and small multipole moments which places severe constraints on the spatial distribution of γ-ray bursts. We discuss a Monte Carlo simulation of the population of galactic neutron stars which can be used to test the hypothesis that γ-ray bursts originate on galactic neutron stars. |
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