Probing Gamma-ray Emission of Geminga & Vela with Non-stationary Models

It is generally believed that the high energy emissions from isolated pulsars are emitted from relativistic electrons/positrons accelerated in outer magnetospheric accelerators (outergaps) via a curvature radiation mechanism, which has a simple exponential cut-off spectrum. However, many gamma-ray p...
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Autor*in:	Yating Chai [verfasserIn] Kwong-Sang Cheng [verfasserIn] Jumpei Takata [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2016

Schlagwörter:	Vela Geminga superposition model

Übergeordnetes Werk:	In: Journal of Astronomy and Space Sciences - Korean Space Science Society (KSSS), 2012, 33(2016), 2, Seite 75-91
Übergeordnetes Werk:	volume:33 ; year:2016 ; number:2 ; pages:75-91

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc Journal toc

DOI / URN:	10.5140/JASS.2016.33.2.75

Katalog-ID:	DOAJ002968800

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520			\|a It is generally believed that the high energy emissions from isolated pulsars are emitted from relativistic electrons/positrons accelerated in outer magnetospheric accelerators (outergaps) via a curvature radiation mechanism, which has a simple exponential cut-off spectrum. However, many gamma-ray pulsars detected by the Fermi LAT (Large Area Telescope) cannot be fitted by simple exponential cut-off spectrum, and instead a sub-exponential is more appropriate. It is proposed that the realistic outergaps are non-stationary, and that the observed spectrum is a superposition of different stationary states that are controlled by the currents injected from the inner and outer boundaries. The Vela and Geminga pulsars have the largest fluxes among all targets observed, which allows us to carry out very detailed phase-resolved spectral analysis. We have divided the Vela and Geminga pulsars into 19 (the off pulse of Vela was not included) and 33 phase bins, respectively. We find that most phase resolved spectra still cannot be fitted by a simple exponential spectrum: in fact, a sub-exponential spectrum is necessary. We conclude that non-stationary states exist even down to the very fine phase bins.
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allfields	10.5140/JASS.2016.33.2.75 doi (DE-627)DOAJ002968800 (DE-599)DOAJe8fb93cb79b74950a8e7517482fca3c0 DE-627 ger DE-627 rakwb eng QB1-991 Yating Chai verfasserin aut Probing Gamma-ray Emission of Geminga & Vela with Non-stationary Models 2016 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier It is generally believed that the high energy emissions from isolated pulsars are emitted from relativistic electrons/positrons accelerated in outer magnetospheric accelerators (outergaps) via a curvature radiation mechanism, which has a simple exponential cut-off spectrum. However, many gamma-ray pulsars detected by the Fermi LAT (Large Area Telescope) cannot be fitted by simple exponential cut-off spectrum, and instead a sub-exponential is more appropriate. It is proposed that the realistic outergaps are non-stationary, and that the observed spectrum is a superposition of different stationary states that are controlled by the currents injected from the inner and outer boundaries. The Vela and Geminga pulsars have the largest fluxes among all targets observed, which allows us to carry out very detailed phase-resolved spectral analysis. We have divided the Vela and Geminga pulsars into 19 (the off pulse of Vela was not included) and 33 phase bins, respectively. We find that most phase resolved spectra still cannot be fitted by a simple exponential spectrum: in fact, a sub-exponential spectrum is necessary. We conclude that non-stationary states exist even down to the very fine phase bins. Vela Geminga superposition model Astronomy Kwong-Sang Cheng verfasserin aut Jumpei Takata verfasserin aut In Journal of Astronomy and Space Sciences Korean Space Science Society (KSSS), 2012 33(2016), 2, Seite 75-91 (DE-627)62761471X (DE-600)2557343-3 20931409 nnns volume:33 year:2016 number:2 pages:75-91 https://doi.org/10.5140/JASS.2016.33.2.75 kostenfrei https://doaj.org/article/e8fb93cb79b74950a8e7517482fca3c0 kostenfrei http://ocean.kisti.re.kr/downfile/volume/kosss/OJOOBS/2016/v33n2/OJOOBS_2016_v33n2_75.pdf kostenfrei https://doaj.org/toc/2093-5587 Journal toc kostenfrei https://doaj.org/toc/2093-1409 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2014 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 33 2016 2 75-91
spelling	10.5140/JASS.2016.33.2.75 doi (DE-627)DOAJ002968800 (DE-599)DOAJe8fb93cb79b74950a8e7517482fca3c0 DE-627 ger DE-627 rakwb eng QB1-991 Yating Chai verfasserin aut Probing Gamma-ray Emission of Geminga & Vela with Non-stationary Models 2016 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier It is generally believed that the high energy emissions from isolated pulsars are emitted from relativistic electrons/positrons accelerated in outer magnetospheric accelerators (outergaps) via a curvature radiation mechanism, which has a simple exponential cut-off spectrum. However, many gamma-ray pulsars detected by the Fermi LAT (Large Area Telescope) cannot be fitted by simple exponential cut-off spectrum, and instead a sub-exponential is more appropriate. It is proposed that the realistic outergaps are non-stationary, and that the observed spectrum is a superposition of different stationary states that are controlled by the currents injected from the inner and outer boundaries. The Vela and Geminga pulsars have the largest fluxes among all targets observed, which allows us to carry out very detailed phase-resolved spectral analysis. We have divided the Vela and Geminga pulsars into 19 (the off pulse of Vela was not included) and 33 phase bins, respectively. We find that most phase resolved spectra still cannot be fitted by a simple exponential spectrum: in fact, a sub-exponential spectrum is necessary. We conclude that non-stationary states exist even down to the very fine phase bins. Vela Geminga superposition model Astronomy Kwong-Sang Cheng verfasserin aut Jumpei Takata verfasserin aut In Journal of Astronomy and Space Sciences Korean Space Science Society (KSSS), 2012 33(2016), 2, Seite 75-91 (DE-627)62761471X (DE-600)2557343-3 20931409 nnns volume:33 year:2016 number:2 pages:75-91 https://doi.org/10.5140/JASS.2016.33.2.75 kostenfrei https://doaj.org/article/e8fb93cb79b74950a8e7517482fca3c0 kostenfrei http://ocean.kisti.re.kr/downfile/volume/kosss/OJOOBS/2016/v33n2/OJOOBS_2016_v33n2_75.pdf kostenfrei https://doaj.org/toc/2093-5587 Journal toc kostenfrei https://doaj.org/toc/2093-1409 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2014 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 33 2016 2 75-91
allfields_unstemmed	10.5140/JASS.2016.33.2.75 doi (DE-627)DOAJ002968800 (DE-599)DOAJe8fb93cb79b74950a8e7517482fca3c0 DE-627 ger DE-627 rakwb eng QB1-991 Yating Chai verfasserin aut Probing Gamma-ray Emission of Geminga & Vela with Non-stationary Models 2016 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier It is generally believed that the high energy emissions from isolated pulsars are emitted from relativistic electrons/positrons accelerated in outer magnetospheric accelerators (outergaps) via a curvature radiation mechanism, which has a simple exponential cut-off spectrum. However, many gamma-ray pulsars detected by the Fermi LAT (Large Area Telescope) cannot be fitted by simple exponential cut-off spectrum, and instead a sub-exponential is more appropriate. It is proposed that the realistic outergaps are non-stationary, and that the observed spectrum is a superposition of different stationary states that are controlled by the currents injected from the inner and outer boundaries. The Vela and Geminga pulsars have the largest fluxes among all targets observed, which allows us to carry out very detailed phase-resolved spectral analysis. We have divided the Vela and Geminga pulsars into 19 (the off pulse of Vela was not included) and 33 phase bins, respectively. We find that most phase resolved spectra still cannot be fitted by a simple exponential spectrum: in fact, a sub-exponential spectrum is necessary. We conclude that non-stationary states exist even down to the very fine phase bins. Vela Geminga superposition model Astronomy Kwong-Sang Cheng verfasserin aut Jumpei Takata verfasserin aut In Journal of Astronomy and Space Sciences Korean Space Science Society (KSSS), 2012 33(2016), 2, Seite 75-91 (DE-627)62761471X (DE-600)2557343-3 20931409 nnns volume:33 year:2016 number:2 pages:75-91 https://doi.org/10.5140/JASS.2016.33.2.75 kostenfrei https://doaj.org/article/e8fb93cb79b74950a8e7517482fca3c0 kostenfrei http://ocean.kisti.re.kr/downfile/volume/kosss/OJOOBS/2016/v33n2/OJOOBS_2016_v33n2_75.pdf kostenfrei https://doaj.org/toc/2093-5587 Journal toc kostenfrei https://doaj.org/toc/2093-1409 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2014 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 33 2016 2 75-91
allfieldsGer	10.5140/JASS.2016.33.2.75 doi (DE-627)DOAJ002968800 (DE-599)DOAJe8fb93cb79b74950a8e7517482fca3c0 DE-627 ger DE-627 rakwb eng QB1-991 Yating Chai verfasserin aut Probing Gamma-ray Emission of Geminga & Vela with Non-stationary Models 2016 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier It is generally believed that the high energy emissions from isolated pulsars are emitted from relativistic electrons/positrons accelerated in outer magnetospheric accelerators (outergaps) via a curvature radiation mechanism, which has a simple exponential cut-off spectrum. However, many gamma-ray pulsars detected by the Fermi LAT (Large Area Telescope) cannot be fitted by simple exponential cut-off spectrum, and instead a sub-exponential is more appropriate. It is proposed that the realistic outergaps are non-stationary, and that the observed spectrum is a superposition of different stationary states that are controlled by the currents injected from the inner and outer boundaries. The Vela and Geminga pulsars have the largest fluxes among all targets observed, which allows us to carry out very detailed phase-resolved spectral analysis. We have divided the Vela and Geminga pulsars into 19 (the off pulse of Vela was not included) and 33 phase bins, respectively. We find that most phase resolved spectra still cannot be fitted by a simple exponential spectrum: in fact, a sub-exponential spectrum is necessary. We conclude that non-stationary states exist even down to the very fine phase bins. Vela Geminga superposition model Astronomy Kwong-Sang Cheng verfasserin aut Jumpei Takata verfasserin aut In Journal of Astronomy and Space Sciences Korean Space Science Society (KSSS), 2012 33(2016), 2, Seite 75-91 (DE-627)62761471X (DE-600)2557343-3 20931409 nnns volume:33 year:2016 number:2 pages:75-91 https://doi.org/10.5140/JASS.2016.33.2.75 kostenfrei https://doaj.org/article/e8fb93cb79b74950a8e7517482fca3c0 kostenfrei http://ocean.kisti.re.kr/downfile/volume/kosss/OJOOBS/2016/v33n2/OJOOBS_2016_v33n2_75.pdf kostenfrei https://doaj.org/toc/2093-5587 Journal toc kostenfrei https://doaj.org/toc/2093-1409 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2014 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 33 2016 2 75-91
allfieldsSound	10.5140/JASS.2016.33.2.75 doi (DE-627)DOAJ002968800 (DE-599)DOAJe8fb93cb79b74950a8e7517482fca3c0 DE-627 ger DE-627 rakwb eng QB1-991 Yating Chai verfasserin aut Probing Gamma-ray Emission of Geminga & Vela with Non-stationary Models 2016 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier It is generally believed that the high energy emissions from isolated pulsars are emitted from relativistic electrons/positrons accelerated in outer magnetospheric accelerators (outergaps) via a curvature radiation mechanism, which has a simple exponential cut-off spectrum. However, many gamma-ray pulsars detected by the Fermi LAT (Large Area Telescope) cannot be fitted by simple exponential cut-off spectrum, and instead a sub-exponential is more appropriate. It is proposed that the realistic outergaps are non-stationary, and that the observed spectrum is a superposition of different stationary states that are controlled by the currents injected from the inner and outer boundaries. The Vela and Geminga pulsars have the largest fluxes among all targets observed, which allows us to carry out very detailed phase-resolved spectral analysis. We have divided the Vela and Geminga pulsars into 19 (the off pulse of Vela was not included) and 33 phase bins, respectively. We find that most phase resolved spectra still cannot be fitted by a simple exponential spectrum: in fact, a sub-exponential spectrum is necessary. We conclude that non-stationary states exist even down to the very fine phase bins. Vela Geminga superposition model Astronomy Kwong-Sang Cheng verfasserin aut Jumpei Takata verfasserin aut In Journal of Astronomy and Space Sciences Korean Space Science Society (KSSS), 2012 33(2016), 2, Seite 75-91 (DE-627)62761471X (DE-600)2557343-3 20931409 nnns volume:33 year:2016 number:2 pages:75-91 https://doi.org/10.5140/JASS.2016.33.2.75 kostenfrei https://doaj.org/article/e8fb93cb79b74950a8e7517482fca3c0 kostenfrei http://ocean.kisti.re.kr/downfile/volume/kosss/OJOOBS/2016/v33n2/OJOOBS_2016_v33n2_75.pdf kostenfrei https://doaj.org/toc/2093-5587 Journal toc kostenfrei https://doaj.org/toc/2093-1409 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2014 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 33 2016 2 75-91
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source	In Journal of Astronomy and Space Sciences 33(2016), 2, Seite 75-91 volume:33 year:2016 number:2 pages:75-91
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topic_facet	Vela Geminga superposition model Astronomy
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authorswithroles_txt_mv	Yating Chai @@aut@@ Kwong-Sang Cheng @@aut@@ Jumpei Takata @@aut@@
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callnumber-first	Q - Science
author	Yating Chai
spellingShingle	Yating Chai misc QB1-991 misc Vela misc Geminga misc superposition model misc Astronomy Probing Gamma-ray Emission of Geminga & Vela with Non-stationary Models
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topic_title	QB1-991 Probing Gamma-ray Emission of Geminga & Vela with Non-stationary Models Vela Geminga superposition model
topic	misc QB1-991 misc Vela misc Geminga misc superposition model misc Astronomy
topic_unstemmed	misc QB1-991 misc Vela misc Geminga misc superposition model misc Astronomy
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title	Probing Gamma-ray Emission of Geminga & Vela with Non-stationary Models
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title_full	Probing Gamma-ray Emission of Geminga & Vela with Non-stationary Models
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title_sort	probing gamma-ray emission of geminga & vela with non-stationary models
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title_auth	Probing Gamma-ray Emission of Geminga & Vela with Non-stationary Models
abstract	It is generally believed that the high energy emissions from isolated pulsars are emitted from relativistic electrons/positrons accelerated in outer magnetospheric accelerators (outergaps) via a curvature radiation mechanism, which has a simple exponential cut-off spectrum. However, many gamma-ray pulsars detected by the Fermi LAT (Large Area Telescope) cannot be fitted by simple exponential cut-off spectrum, and instead a sub-exponential is more appropriate. It is proposed that the realistic outergaps are non-stationary, and that the observed spectrum is a superposition of different stationary states that are controlled by the currents injected from the inner and outer boundaries. The Vela and Geminga pulsars have the largest fluxes among all targets observed, which allows us to carry out very detailed phase-resolved spectral analysis. We have divided the Vela and Geminga pulsars into 19 (the off pulse of Vela was not included) and 33 phase bins, respectively. We find that most phase resolved spectra still cannot be fitted by a simple exponential spectrum: in fact, a sub-exponential spectrum is necessary. We conclude that non-stationary states exist even down to the very fine phase bins.
abstractGer	It is generally believed that the high energy emissions from isolated pulsars are emitted from relativistic electrons/positrons accelerated in outer magnetospheric accelerators (outergaps) via a curvature radiation mechanism, which has a simple exponential cut-off spectrum. However, many gamma-ray pulsars detected by the Fermi LAT (Large Area Telescope) cannot be fitted by simple exponential cut-off spectrum, and instead a sub-exponential is more appropriate. It is proposed that the realistic outergaps are non-stationary, and that the observed spectrum is a superposition of different stationary states that are controlled by the currents injected from the inner and outer boundaries. The Vela and Geminga pulsars have the largest fluxes among all targets observed, which allows us to carry out very detailed phase-resolved spectral analysis. We have divided the Vela and Geminga pulsars into 19 (the off pulse of Vela was not included) and 33 phase bins, respectively. We find that most phase resolved spectra still cannot be fitted by a simple exponential spectrum: in fact, a sub-exponential spectrum is necessary. We conclude that non-stationary states exist even down to the very fine phase bins.
abstract_unstemmed	It is generally believed that the high energy emissions from isolated pulsars are emitted from relativistic electrons/positrons accelerated in outer magnetospheric accelerators (outergaps) via a curvature radiation mechanism, which has a simple exponential cut-off spectrum. However, many gamma-ray pulsars detected by the Fermi LAT (Large Area Telescope) cannot be fitted by simple exponential cut-off spectrum, and instead a sub-exponential is more appropriate. It is proposed that the realistic outergaps are non-stationary, and that the observed spectrum is a superposition of different stationary states that are controlled by the currents injected from the inner and outer boundaries. The Vela and Geminga pulsars have the largest fluxes among all targets observed, which allows us to carry out very detailed phase-resolved spectral analysis. We have divided the Vela and Geminga pulsars into 19 (the off pulse of Vela was not included) and 33 phase bins, respectively. We find that most phase resolved spectra still cannot be fitted by a simple exponential spectrum: in fact, a sub-exponential spectrum is necessary. We conclude that non-stationary states exist even down to the very fine phase bins.
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title_short	Probing Gamma-ray Emission of Geminga & Vela with Non-stationary Models
url	https://doi.org/10.5140/JASS.2016.33.2.75 https://doaj.org/article/e8fb93cb79b74950a8e7517482fca3c0 http://ocean.kisti.re.kr/downfile/volume/kosss/OJOOBS/2016/v33n2/OJOOBS_2016_v33n2_75.pdf https://doaj.org/toc/2093-5587 https://doaj.org/toc/2093-1409
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up_date	2024-07-03T15:10:52.011Z
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Probing Gamma-ray Emission of Geminga & Vela with Non-stationary Models

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