XMM–Newton observations of PSR B1259−63 near the 2004 periastron passage
Identifieur interne : 009864 ( Main/Exploration ); précédent : 009863; suivant : 009865XMM–Newton observations of PSR B1259−63 near the 2004 periastron passage
Auteurs : M. Chernyakova [Suisse, Russie] ; A. Neronov [Suisse] ; A. Lutovinov [Russie] ; J. Rodriguez [France] ; S. Johnston [Australie]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2006-04.
Descripteurs français
- Pascal (Inist)
English descriptors
- KwdEn :
- Asca, Asca observations, Bepposax, Binary X ray source, Bottom panel, Bremsstrahlung, Bremsstrahlung emission, Bremsstrahlung luminosity, Chernyakova, Chernyakova illarionov, Contact surface, Cosmic x-ray sources, Coulomb, Curves show, Disc, Disc passage, Emission region, Energy range, Gamma emission, Gamma radiation, Inverse bremsstrahlung, Journal compilation, Kaspi, Light curve, Light curves, Luminosity, MeV range, Mnras, Models, Normal distribution, Observations show, Orbital, Orbital phase, Orbits, Periastron, Periastron passage, Photon, Photon index, Pulsar, Pulsar orbit, Pulsar wind, Pulsar wind electrons, Pulsars, Radio emission, Radio light curves, Radio synchrotron emission, Rapid growth, Second time, Source position, Spectral analysis, Spectral index, Spectral parameters, Spectral slope, Star disc, Stellar, Stellar wind, Stellar winds, Synchrotron, Synchrotron cooling time, Synchrotron emission, Synchrotron radiation, Tavani, Tavani arons, Timing analysis, Unpulsed, Unpulsed radio emission, Upper limit, X ray emission, X-ray binary stars, X-ray spectra.
- Teeft :
- Asca, Asca observations, Bepposax, Bottom panel, Bremsstrahlung, Bremsstrahlung emission, Bremsstrahlung luminosity, Chernyakova, Chernyakova illarionov, Contact surface, Coulomb, Curves show, Disc, Disc passage, Emission region, Energy range, Journal compilation, Kaspi, Light curve, Light curves, Luminosity, Mnras, Observations show, Orbital, Orbital phase, Periastron, Periastron passage, Photon, Photon index, Pulsar, Pulsar orbit, Pulsar wind, Pulsar wind electrons, Radio emission, Radio light curves, Radio synchrotron emission, Rapid growth, Second time, Source position, Spectral analysis, Spectral index, Spectral parameters, Spectral slope, Star disc, Stellar, Stellar wind, Synchrotron, Synchrotron cooling time, Synchrotron emission, Tavani, Tavani arons, Timing analysis, Unpulsed, Unpulsed radio emission, Upper limit.
Abstract
PSR B1259−63 is in a highly eccentric 3.4‐yr orbit with a Be star and crosses the Be star disc twice per orbit, just prior to and just after periastron. Unpulsed radio, X‐ray and gamma‐ray emission observed from the binary system is thought to be due to the collision of pulsar wind with the wind of Be star. We present here the results of new XMM–Newton observations of the PSR B1259−63 system during the beginning of 2004 as the pulsar approached the disc of the Be star. We combine these results with the earlier unpublished X‐ray data from BeppoSAX and XMM–Newton as well as with the ASCA data. The detailed X‐ray light curve of the system shows that the pulsar passes (twice per orbit) through a well‐defined Gaussian‐profile disc with the half‐opening angle (projected on the pulsar orbit plane) . The intersection of the disc middle plane with the pulsar orbital plane is inclined at θdisc≃ 70° to the major axis of the pulsar orbit. Comparing the X‐ray light curve to the TeV light curve of the the system, we find that the increase of the TeV flux some 10–100 d after the periastron passage is unambiguously related to the disc passage. At the moment of entrance to the disc, the X‐ray photon index hardens from Γ≃ 1.8 up to ≃1.2 before returning to the steeper value Γ≥ 1.5. Such behaviour is not easily accounted for by the model in which the X‐ray emission is synchrotron emission from the shocked pulsar wind. We argue that the observed hardening of the X‐ray spectrum is due to the inverse‐Compton or bremsstrahlung emission from 10–100 MeV electrons responsible for the radio synchrotron emission.
Url:
- https://api.istex.fr/document/7DBC7AF9072A8812909F47AFD0DC7E79E292236F/fulltext/pdf
- https://api.istex.fr/document/FC8148A512BB7EEDF4EE43B8D194B178F04497B7/fulltext/pdf
DOI: 10.1111/j.1365-2966.2005.10039.x
Affiliations:
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Chernyakova</name><affiliation wicri:level="1"><country xml:lang="fr">Suisse</country><wicri:regionArea>INTEGRAL Science Data Center, Chemin d'Écogia 16, 1290 Versoix</wicri:regionArea><wicri:noRegion>1290 Versoix</wicri:noRegion></affiliation><affiliation wicri:level="1"><country xml:lang="fr">Suisse</country><wicri:regionArea>Geneva Observatory, 51 ch. des Maillettes, CH‐1290 Sauverny</wicri:regionArea><wicri:noRegion>CH‐1290 Sauverny</wicri:noRegion></affiliation><affiliation wicri:level="3"><country xml:lang="fr">Russie</country><wicri:regionArea>E‐mail: M. Chernyakova is on leave from Astro Space Center of the P. N. Lebedev Physical Institute, Moscow</wicri:regionArea><placeName><settlement type="city">Moscou</settlement><region>District fédéral central</region></placeName></affiliation><affiliation wicri:level="1"><country wicri:rule="url">Suisse</country></affiliation></author><author><name sortKey="Neronov, A" sort="Neronov, A" uniqKey="Neronov A" first="A." last="Neronov">A. Neronov</name><affiliation wicri:level="1"><country xml:lang="fr">Suisse</country><wicri:regionArea>INTEGRAL Science Data Center, Chemin d'Écogia 16, 1290 Versoix</wicri:regionArea><wicri:noRegion>1290 Versoix</wicri:noRegion></affiliation><affiliation wicri:level="1"><country xml:lang="fr">Suisse</country><wicri:regionArea>Geneva Observatory, 51 ch. des Maillettes, CH‐1290 Sauverny</wicri:regionArea><wicri:noRegion>CH‐1290 Sauverny</wicri:noRegion></affiliation></author><author><name sortKey="Lutovinov, A" sort="Lutovinov, A" uniqKey="Lutovinov A" first="A." last="Lutovinov">A. Lutovinov</name><affiliation wicri:level="1"><country xml:lang="fr">Russie</country><wicri:regionArea>Space Research Institute, 84/32 Profsoyuznaya Street, Moscow 117997</wicri:regionArea><placeName><settlement type="city">Moscou</settlement><region>District fédéral central</region></placeName></affiliation></author><author><name sortKey="Rodriguez, J" sort="Rodriguez, J" uniqKey="Rodriguez J" first="J." last="Rodriguez">J. Rodriguez</name><affiliation wicri:level="3"><country xml:lang="fr">France</country><wicri:regionArea>CEA Saclay, DSM/DAPNIA/Service d'Astrophysique (CNRS UMR 7158 AIM), 91191 Gif sur Yvette</wicri:regionArea><placeName><region type="region" nuts="2">Île-de-France</region><settlement type="city">Gif sur Yvette</settlement></placeName></affiliation></author><author><name sortKey="Johnston, S" sort="Johnston, S" uniqKey="Johnston S" first="S." last="Johnston">S. Johnston</name><affiliation wicri:level="1"><country xml:lang="fr">Australie</country><wicri:regionArea>Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710</wicri:regionArea><wicri:noRegion>NSW 1710</wicri:noRegion></affiliation></author></analytic><monogr></monogr><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title><idno type="ISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><imprint><biblScope unit="vol">367</biblScope><biblScope unit="issue">3</biblScope><biblScope unit="page" from="1201">1201</biblScope><biblScope unit="page" to="1208">1208</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace> 23 Ainslie Place , Edinburgh EH3 6AJ , UK . Telephone (0131) 226 7232 Fax (0131) 226 3803 </pubPlace><date type="published" when="2006-04">2006-04</date></imprint><idno type="ISSN">0035-8711</idno></series></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Asca</term><term>Asca observations</term><term>Bepposax</term><term>Binary X ray source</term><term>Bottom panel</term><term>Bremsstrahlung</term><term>Bremsstrahlung emission</term><term>Bremsstrahlung luminosity</term><term>Chernyakova</term><term>Chernyakova illarionov</term><term>Contact surface</term><term>Cosmic x-ray sources</term><term>Coulomb</term><term>Curves show</term><term>Disc</term><term>Disc passage</term><term>Emission region</term><term>Energy range</term><term>Gamma emission</term><term>Gamma radiation</term><term>Inverse bremsstrahlung</term><term>Journal compilation</term><term>Kaspi</term><term>Light curve</term><term>Light curves</term><term>Luminosity</term><term>MeV range</term><term>Mnras</term><term>Models</term><term>Normal distribution</term><term>Observations show</term><term>Orbital</term><term>Orbital phase</term><term>Orbits</term><term>Periastron</term><term>Periastron passage</term><term>Photon</term><term>Photon index</term><term>Pulsar</term><term>Pulsar orbit</term><term>Pulsar wind</term><term>Pulsar wind electrons</term><term>Pulsars</term><term>Radio emission</term><term>Radio light curves</term><term>Radio synchrotron emission</term><term>Rapid growth</term><term>Second time</term><term>Source position</term><term>Spectral analysis</term><term>Spectral index</term><term>Spectral parameters</term><term>Spectral slope</term><term>Star disc</term><term>Stellar</term><term>Stellar wind</term><term>Stellar winds</term><term>Synchrotron</term><term>Synchrotron cooling time</term><term>Synchrotron emission</term><term>Synchrotron radiation</term><term>Tavani</term><term>Tavani arons</term><term>Timing analysis</term><term>Unpulsed</term><term>Unpulsed radio emission</term><term>Upper limit</term><term>X ray emission</term><term>X-ray binary stars</term><term>X-ray spectra</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Binaire RX</term><term>Courbe lumière</term><term>Domaine énergie MeV</term><term>Emission RX</term><term>Emission gamma</term><term>Emission radioélectrique</term><term>Loi normale</term><term>Modèle</term><term>Orbite</term><term>Pulsar</term><term>Périastre</term><term>Rayonnement freinage inverse</term><term>Rayonnement gamma</term><term>Rayonnement synchrotron</term><term>Source RX binaire</term><term>Source RX cosmique</term><term>Spectre RX</term><term>Vent stellaire</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>Asca</term><term>Asca observations</term><term>Bepposax</term><term>Bottom panel</term><term>Bremsstrahlung</term><term>Bremsstrahlung emission</term><term>Bremsstrahlung luminosity</term><term>Chernyakova</term><term>Chernyakova illarionov</term><term>Contact surface</term><term>Coulomb</term><term>Curves show</term><term>Disc</term><term>Disc passage</term><term>Emission region</term><term>Energy range</term><term>Journal compilation</term><term>Kaspi</term><term>Light curve</term><term>Light curves</term><term>Luminosity</term><term>Mnras</term><term>Observations show</term><term>Orbital</term><term>Orbital phase</term><term>Periastron</term><term>Periastron passage</term><term>Photon</term><term>Photon index</term><term>Pulsar</term><term>Pulsar orbit</term><term>Pulsar wind</term><term>Pulsar wind electrons</term><term>Radio emission</term><term>Radio light curves</term><term>Radio synchrotron emission</term><term>Rapid growth</term><term>Second time</term><term>Source position</term><term>Spectral analysis</term><term>Spectral index</term><term>Spectral parameters</term><term>Spectral slope</term><term>Star disc</term><term>Stellar</term><term>Stellar wind</term><term>Synchrotron</term><term>Synchrotron cooling time</term><term>Synchrotron emission</term><term>Tavani</term><term>Tavani arons</term><term>Timing analysis</term><term>Unpulsed</term><term>Unpulsed radio emission</term><term>Upper limit</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">PSR B1259−63 is in a highly eccentric 3.4‐yr orbit with a Be star and crosses the Be star disc twice per orbit, just prior to and just after periastron. Unpulsed radio, X‐ray and gamma‐ray emission observed from the binary system is thought to be due to the collision of pulsar wind with the wind of Be star. We present here the results of new XMM–Newton observations of the PSR B1259−63 system during the beginning of 2004 as the pulsar approached the disc of the Be star. We combine these results with the earlier unpublished X‐ray data from BeppoSAX and XMM–Newton as well as with the ASCA data. The detailed X‐ray light curve of the system shows that the pulsar passes (twice per orbit) through a well‐defined Gaussian‐profile disc with the half‐opening angle (projected on the pulsar orbit plane) . The intersection of the disc middle plane with the pulsar orbital plane is inclined at θdisc≃ 70° to the major axis of the pulsar orbit. Comparing the X‐ray light curve to the TeV light curve of the the system, we find that the increase of the TeV flux some 10–100 d after the periastron passage is unambiguously related to the disc passage. At the moment of entrance to the disc, the X‐ray photon index hardens from Γ≃ 1.8 up to ≃1.2 before returning to the steeper value Γ≥ 1.5. Such behaviour is not easily accounted for by the model in which the X‐ray emission is synchrotron emission from the shocked pulsar wind. We argue that the observed hardening of the X‐ray spectrum is due to the inverse‐Compton or bremsstrahlung emission from 10–100 MeV electrons responsible for the radio synchrotron emission.</div></front></TEI><affiliations><list><country><li>Australie</li><li>France</li><li>Russie</li><li>Suisse</li></country><region><li>District fédéral central</li><li>Île-de-France</li></region><settlement><li>Gif sur Yvette</li><li>Moscou</li></settlement></list><tree><country name="Suisse"><noRegion><name sortKey="Chernyakova, M" sort="Chernyakova, M" uniqKey="Chernyakova M" first="M." last="Chernyakova">M. Chernyakova</name></noRegion><name sortKey="Chernyakova, M" sort="Chernyakova, M" uniqKey="Chernyakova M" first="M." last="Chernyakova">M. Chernyakova</name><name sortKey="Chernyakova, M" sort="Chernyakova, M" uniqKey="Chernyakova M" first="M." last="Chernyakova">M. Chernyakova</name><name sortKey="Neronov, A" sort="Neronov, A" uniqKey="Neronov A" first="A." last="Neronov">A. Neronov</name><name sortKey="Neronov, A" sort="Neronov, A" uniqKey="Neronov A" first="A." last="Neronov">A. Neronov</name></country><country name="Russie"><region name="District fédéral central"><name sortKey="Chernyakova, M" sort="Chernyakova, M" uniqKey="Chernyakova M" first="M." last="Chernyakova">M. Chernyakova</name></region><name sortKey="Lutovinov, A" sort="Lutovinov, A" uniqKey="Lutovinov A" first="A." last="Lutovinov">A. Lutovinov</name></country><country name="France"><region name="Île-de-France"><name sortKey="Rodriguez, J" sort="Rodriguez, J" uniqKey="Rodriguez J" first="J." last="Rodriguez">J. Rodriguez</name></region></country><country name="Australie"><noRegion><name sortKey="Johnston, S" sort="Johnston, S" uniqKey="Johnston S" first="S." last="Johnston">S. Johnston</name></noRegion></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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