Spectral and timing properties of the accreting X-ray millisecond pulsar IGR J17511-3057
Identifieur interne : 004413 ( PascalFrancis/Curation ); précédent : 004412; suivant : 004414Spectral and timing properties of the accreting X-ray millisecond pulsar IGR J17511-3057
Auteurs : M. Falanga [Suisse] ; L. Kuiper [Pays-Bas] ; J. Poutanen [Finlande] ; D. K. Galloway [Australie] ; E. W. Bonning [États-Unis] ; E. Bozzo [Suisse] ; A. Goldwurm [France] ; W. Hermsen [Pays-Bas] ; L. Stella [Italie]Source :
- Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2011.
Descripteurs français
- Pascal (Inist)
- Propriété spectrale, Timing, Pulsar RX, Source RX transitoire, Pulsar milliseconde, Sursaut RX, Domaine énergie keV, Courbe lumière, Forme impulsion, Température électron, Epaisseur optique, Plasma, Température photon, Diffusion optique, Modèle, Instabilité, Pulsation RX, Métallicité, Etoile neutron, Binaire RX, Source RX binaire, Source RX cosmique.
English descriptors
- KwdEn :
- Binary X ray source, Cosmic x-ray sources, Electron temperature, Instability, Light curves, Metallicity, Millisecond pulsar, Models, Neutron stars, Optical scattering, Optical thickness, Photon temperature, Plasma, Pulse shape, Spectral properties, Timing, Transient X ray source, X ray burst, X ray pulsar, X ray pulsation, X-ray binary stars, keV range.
Abstract
Context. IGR J17511-3057 is the second X-ray transient accreting millisecond pulsar discovered by INTEGRAL. It was in outburst for about a month beginning on September 13, 2009. Aims. We analyze the spectral and timing properties of the object and the characteristics of X-ray bursts with the aim to constrain the physical processes responsible for the X-ray production in this class of sources. Methods. We studied the broad-band spectrum of the persistent emission in the 0.8-300 keV energy band using simultaneous INTEGRAL, RXTE and Swift data obtained in September 2009. We also describe the timing properties in the 2-120 keV energy range such as the outburst light curve, pulse profile, pulsed fraction, pulsed emission, and time lags, and moreover study the properties of X-ray bursts discovered by RXTE and INTEGRAL and the recurrence time. Results. The broad-band average spectrum is well described by thermal Comptonization with an electron temperature of kTe ∼ 25 keV, soft seed photons of kTbb ∼ 0.6 keV, and Thomson optical depth τT ∼ 2 in a slab geometry. During the outburst the spectrum stays remarkably stable with plasma and soft seed photon temperatures and scattering optical depth being constant within errors. We fitted the outburst profile with the exponential model, and using the disk instability model we inferred the outer disk radius to be (4.8-5.4) x 1010 cm. The INTEGRAL and RXTE data reveal the X-ray pulsation at a period of 4.08 milliseconds up to ∼120 keV. The pulsed fraction is shown to decrease from ∼22% at 3 keV to a constant pulsed fraction of ∼17-18% between 7-30 keV, and then to decrease again to ∼13% at 60 keV. The nearly sinusoidal pulses show soft lags that monotonically increase with energy to about 0.2 ms at 10-20 keV similar to those observed in other accreting pulsars. The short burst profiles indicate hydrogen-poor material at ignition, which suggests either that the accreted material is hydrogen-deficient, or that the CNO metallicity is up to a factor of 2 times solar. However, the variation of the burst recurrence time as a function of m (inferred from the X-ray flux) is much smaller than predicted by helium-ignition models.
| pA |
|
|---|
Links toward previous steps (curation, corpus...)
- to stream PascalFrancis, to step Corpus: Pour aller vers cette notice dans l'étape Curation :001B31
Links to Exploration step
Pascal:11-0310959Le document en format XML
<record><TEI><teiHeader><fileDesc><titleStmt><title xml:lang="en" level="a">Spectral and timing properties of the accreting X-ray millisecond pulsar IGR J17511-3057</title><author><name sortKey="Falanga, M" sort="Falanga, M" uniqKey="Falanga M" first="M." last="Falanga">M. Falanga</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>International Space Science Institute (ISSI), Hallerstrasse 6</s1><s2>3012 Bern</s2><s3>CHE</s3><sZ>1 aut.</sZ></inist:fA14><country>Suisse</country></affiliation></author><author><name sortKey="Kuiper, L" sort="Kuiper, L" uniqKey="Kuiper L" first="L." last="Kuiper">L. Kuiper</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>SRON - Netherlands Institute for Space Research, Sorbonnelaan 2</s1><s2>3584 CA, Utrecht</s2><s3>NLD</s3><sZ>2 aut.</sZ><sZ>8 aut.</sZ></inist:fA14><country>Pays-Bas</country></affiliation></author><author><name sortKey="Poutanen, J" sort="Poutanen, J" uniqKey="Poutanen J" first="J." last="Poutanen">J. Poutanen</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Astronomy Division, Department of Physics, PO Box 3000, 90014 University of Oulu</s1><s3>FIN</s3><sZ>3 aut.</sZ></inist:fA14><country>Finlande</country></affiliation></author><author><name sortKey="Galloway, D K" sort="Galloway, D K" uniqKey="Galloway D" first="D. K." last="Galloway">D. K. Galloway</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>School of Physics and School of Mathematical Sciences, Monash University</s1><s2>VIC 3800</s2><s3>AUS</s3><sZ>4 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Bonning, E W" sort="Bonning, E W" uniqKey="Bonning E" first="E. W." last="Bonning">E. W. Bonning</name><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Department of Physics and Yale Center for Astronomy and Astrophysics, Yale University, PO Box 208121</s1><s2>New Haven, CT 06520-8121</s2><s3>USA</s3><sZ>5 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Bozzo, E" sort="Bozzo, E" uniqKey="Bozzo E" first="E." last="Bozzo">E. Bozzo</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>ISDC, Data centre for astrophysics, University of Geneva, Chemin d'Écogia 16</s1><s2>1290 Versoix</s2><s3>CHE</s3><sZ>6 aut.</sZ></inist:fA14><country>Suisse</country></affiliation></author><author><name sortKey="Goldwurm, A" sort="Goldwurm, A" uniqKey="Goldwurm A" first="A." last="Goldwurm">A. Goldwurm</name><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>Service dAstrophysique (SAp), IRFU/DSM/CEA-Saclay</s1><s2>91191 Gif-sur-Yvette</s2><s3>FRA</s3><sZ>7 aut.</sZ></inist:fA14><country>France</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Unité mixte de recherche Astroparticule et Cosmologie, 10 rue Alice Domon et Leonie Duquet</s1><s2>75205 Paris</s2><s3>FRA</s3><sZ>7 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Hermsen, W" sort="Hermsen, W" uniqKey="Hermsen W" first="W." last="Hermsen">W. Hermsen</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>SRON - Netherlands Institute for Space Research, Sorbonnelaan 2</s1><s2>3584 CA, Utrecht</s2><s3>NLD</s3><sZ>2 aut.</sZ><sZ>8 aut.</sZ></inist:fA14><country>Pays-Bas</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="09"><s1>Astronomical Institute "Anton Pannekoek", University of Amsterdam, Science Park 904</s1><s2>1098 XH, Amsterdam</s2><s3>NLD</s3><sZ>8 aut.</sZ></inist:fA14><country>Pays-Bas</country></affiliation></author><author><name sortKey="Stella, L" sort="Stella, L" uniqKey="Stella L" first="L." last="Stella">L. Stella</name><affiliation wicri:level="1"><inist:fA14 i1="10"><s1>INAF - Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio Catone</s1><s2>Roma</s2><s3>ITA</s3><sZ>9 aut.</sZ></inist:fA14><country>Italie</country></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">11-0310959</idno><date when="2011">2011</date><idno type="stanalyst">PASCAL 11-0310959 INIST</idno><idno type="RBID">Pascal:11-0310959</idno><idno type="wicri:Area/PascalFrancis/Corpus">001B31</idno><idno type="wicri:Area/PascalFrancis/Curation">004413</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Spectral and timing properties of the accreting X-ray millisecond pulsar IGR J17511-3057</title><author><name sortKey="Falanga, M" sort="Falanga, M" uniqKey="Falanga M" first="M." last="Falanga">M. Falanga</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>International Space Science Institute (ISSI), Hallerstrasse 6</s1><s2>3012 Bern</s2><s3>CHE</s3><sZ>1 aut.</sZ></inist:fA14><country>Suisse</country></affiliation></author><author><name sortKey="Kuiper, L" sort="Kuiper, L" uniqKey="Kuiper L" first="L." last="Kuiper">L. Kuiper</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>SRON - Netherlands Institute for Space Research, Sorbonnelaan 2</s1><s2>3584 CA, Utrecht</s2><s3>NLD</s3><sZ>2 aut.</sZ><sZ>8 aut.</sZ></inist:fA14><country>Pays-Bas</country></affiliation></author><author><name sortKey="Poutanen, J" sort="Poutanen, J" uniqKey="Poutanen J" first="J." last="Poutanen">J. Poutanen</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Astronomy Division, Department of Physics, PO Box 3000, 90014 University of Oulu</s1><s3>FIN</s3><sZ>3 aut.</sZ></inist:fA14><country>Finlande</country></affiliation></author><author><name sortKey="Galloway, D K" sort="Galloway, D K" uniqKey="Galloway D" first="D. K." last="Galloway">D. K. Galloway</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>School of Physics and School of Mathematical Sciences, Monash University</s1><s2>VIC 3800</s2><s3>AUS</s3><sZ>4 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Bonning, E W" sort="Bonning, E W" uniqKey="Bonning E" first="E. W." last="Bonning">E. W. Bonning</name><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Department of Physics and Yale Center for Astronomy and Astrophysics, Yale University, PO Box 208121</s1><s2>New Haven, CT 06520-8121</s2><s3>USA</s3><sZ>5 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Bozzo, E" sort="Bozzo, E" uniqKey="Bozzo E" first="E." last="Bozzo">E. Bozzo</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>ISDC, Data centre for astrophysics, University of Geneva, Chemin d'Écogia 16</s1><s2>1290 Versoix</s2><s3>CHE</s3><sZ>6 aut.</sZ></inist:fA14><country>Suisse</country></affiliation></author><author><name sortKey="Goldwurm, A" sort="Goldwurm, A" uniqKey="Goldwurm A" first="A." last="Goldwurm">A. Goldwurm</name><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>Service dAstrophysique (SAp), IRFU/DSM/CEA-Saclay</s1><s2>91191 Gif-sur-Yvette</s2><s3>FRA</s3><sZ>7 aut.</sZ></inist:fA14><country>France</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Unité mixte de recherche Astroparticule et Cosmologie, 10 rue Alice Domon et Leonie Duquet</s1><s2>75205 Paris</s2><s3>FRA</s3><sZ>7 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Hermsen, W" sort="Hermsen, W" uniqKey="Hermsen W" first="W." last="Hermsen">W. Hermsen</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>SRON - Netherlands Institute for Space Research, Sorbonnelaan 2</s1><s2>3584 CA, Utrecht</s2><s3>NLD</s3><sZ>2 aut.</sZ><sZ>8 aut.</sZ></inist:fA14><country>Pays-Bas</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="09"><s1>Astronomical Institute "Anton Pannekoek", University of Amsterdam, Science Park 904</s1><s2>1098 XH, Amsterdam</s2><s3>NLD</s3><sZ>8 aut.</sZ></inist:fA14><country>Pays-Bas</country></affiliation></author><author><name sortKey="Stella, L" sort="Stella, L" uniqKey="Stella L" first="L." last="Stella">L. Stella</name><affiliation wicri:level="1"><inist:fA14 i1="10"><s1>INAF - Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio Catone</s1><s2>Roma</s2><s3>ITA</s3><sZ>9 aut.</sZ></inist:fA14><country>Italie</country></affiliation></author></analytic><series><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title><title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title><idno type="ISSN">0004-6361</idno><imprint><date when="2011">2011</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title><title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title><idno type="ISSN">0004-6361</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Binary X ray source</term><term>Cosmic x-ray sources</term><term>Electron temperature</term><term>Instability</term><term>Light curves</term><term>Metallicity</term><term>Millisecond pulsar</term><term>Models</term><term>Neutron stars</term><term>Optical scattering</term><term>Optical thickness</term><term>Photon temperature</term><term>Plasma</term><term>Pulse shape</term><term>Spectral properties</term><term>Timing</term><term>Transient X ray source</term><term>X ray burst</term><term>X ray pulsar</term><term>X ray pulsation</term><term>X-ray binary stars</term><term>keV range</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Propriété spectrale</term><term>Timing</term><term>Pulsar RX</term><term>Source RX transitoire</term><term>Pulsar milliseconde</term><term>Sursaut RX</term><term>Domaine énergie keV</term><term>Courbe lumière</term><term>Forme impulsion</term><term>Température électron</term><term>Epaisseur optique</term><term>Plasma</term><term>Température photon</term><term>Diffusion optique</term><term>Modèle</term><term>Instabilité</term><term>Pulsation RX</term><term>Métallicité</term><term>Etoile neutron</term><term>Binaire RX</term><term>Source RX binaire</term><term>Source RX cosmique</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">Context. IGR J17511-3057 is the second X-ray transient accreting millisecond pulsar discovered by INTEGRAL. It was in outburst for about a month beginning on September 13, 2009. Aims. We analyze the spectral and timing properties of the object and the characteristics of X-ray bursts with the aim to constrain the physical processes responsible for the X-ray production in this class of sources. Methods. We studied the broad-band spectrum of the persistent emission in the 0.8-300 keV energy band using simultaneous INTEGRAL, RXTE and Swift data obtained in September 2009. We also describe the timing properties in the 2-120 keV energy range such as the outburst light curve, pulse profile, pulsed fraction, pulsed emission, and time lags, and moreover study the properties of X-ray bursts discovered by RXTE and INTEGRAL and the recurrence time. Results. The broad-band average spectrum is well described by thermal Comptonization with an electron temperature of kT<sub>e</sub> ∼ 25 keV, soft seed photons of kT<sub>bb</sub> ∼ 0.6 keV, and Thomson optical depth τ<sub>T</sub> ∼ 2 in a slab geometry. During the outburst the spectrum stays remarkably stable with plasma and soft seed photon temperatures and scattering optical depth being constant within errors. We fitted the outburst profile with the exponential model, and using the disk instability model we inferred the outer disk radius to be (4.8-5.4) x 10<sup>10</sup> cm. The INTEGRAL and RXTE data reveal the X-ray pulsation at a period of 4.08 milliseconds up to ∼120 keV. The pulsed fraction is shown to decrease from ∼22% at 3 keV to a constant pulsed fraction of ∼17-18% between 7-30 keV, and then to decrease again to ∼13% at 60 keV. The nearly sinusoidal pulses show soft lags that monotonically increase with energy to about 0.2 ms at 10-20 keV similar to those observed in other accreting pulsars. The short burst profiles indicate hydrogen-poor material at ignition, which suggests either that the accreted material is hydrogen-deficient, or that the CNO metallicity is up to a factor of 2 times solar. However, the variation of the burst recurrence time as a function of m (inferred from the X-ray flux) is much smaller than predicted by helium-ignition models.</div></front></TEI><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0004-6361</s0></fA01><fA02 i1="01"><s0>AAEJAF</s0></fA02><fA03 i2="1"><s0>Astron. astrophys. : (Berl., Print)</s0></fA03><fA05><s2>529</s2></fA05><fA06><s3>p. 1</s3></fA06><fA08 i1="01" i2="1" l="ENG"><s1>Spectral and timing properties of the accreting X-ray millisecond pulsar IGR J17511-3057</s1></fA08><fA11 i1="01" i2="1"><s1>FALANGA (M.)</s1></fA11><fA11 i1="02" i2="1"><s1>KUIPER (L.)</s1></fA11><fA11 i1="03" i2="1"><s1>POUTANEN (J.)</s1></fA11><fA11 i1="04" i2="1"><s1>GALLOWAY (D. K.)</s1></fA11><fA11 i1="05" i2="1"><s1>BONNING (E. W.)</s1></fA11><fA11 i1="06" i2="1"><s1>BOZZO (E.)</s1></fA11><fA11 i1="07" i2="1"><s1>GOLDWURM (A.)</s1></fA11><fA11 i1="08" i2="1"><s1>HERMSEN (W.)</s1></fA11><fA11 i1="09" i2="1"><s1>STELLA (L.)</s1></fA11><fA14 i1="01"><s1>International Space Science Institute (ISSI), Hallerstrasse 6</s1><s2>3012 Bern</s2><s3>CHE</s3><sZ>1 aut.</sZ></fA14><fA14 i1="02"><s1>SRON - Netherlands Institute for Space Research, Sorbonnelaan 2</s1><s2>3584 CA, Utrecht</s2><s3>NLD</s3><sZ>2 aut.</sZ><sZ>8 aut.</sZ></fA14><fA14 i1="03"><s1>Astronomy Division, Department of Physics, PO Box 3000, 90014 University of Oulu</s1><s3>FIN</s3><sZ>3 aut.</sZ></fA14><fA14 i1="04"><s1>School of Physics and School of Mathematical Sciences, Monash University</s1><s2>VIC 3800</s2><s3>AUS</s3><sZ>4 aut.</sZ></fA14><fA14 i1="05"><s1>Department of Physics and Yale Center for Astronomy and Astrophysics, Yale University, PO Box 208121</s1><s2>New Haven, CT 06520-8121</s2><s3>USA</s3><sZ>5 aut.</sZ></fA14><fA14 i1="06"><s1>ISDC, Data centre for astrophysics, University of Geneva, Chemin d'Écogia 16</s1><s2>1290 Versoix</s2><s3>CHE</s3><sZ>6 aut.</sZ></fA14><fA14 i1="07"><s1>Service dAstrophysique (SAp), IRFU/DSM/CEA-Saclay</s1><s2>91191 Gif-sur-Yvette</s2><s3>FRA</s3><sZ>7 aut.</sZ></fA14><fA14 i1="08"><s1>Unité mixte de recherche Astroparticule et Cosmologie, 10 rue Alice Domon et Leonie Duquet</s1><s2>75205 Paris</s2><s3>FRA</s3><sZ>7 aut.</sZ></fA14><fA14 i1="09"><s1>Astronomical Institute "Anton Pannekoek", University of Amsterdam, Science Park 904</s1><s2>1098 XH, Amsterdam</s2><s3>NLD</s3><sZ>8 aut.</sZ></fA14><fA14 i1="10"><s1>INAF - Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio Catone</s1><s2>Roma</s2><s3>ITA</s3><sZ>9 aut.</sZ></fA14><fA20><s2>529A68.1-529A68.11</s2></fA20><fA21><s1>2011</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>14176</s2><s5>354000189922800640</s5></fA43><fA44><s0>0000</s0><s1>© 2011 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>3/4 p.</s0></fA45><fA47 i1="01" i2="1"><s0>11-0310959</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>Astronomy and astrophysics : (Berlin. Print)</s0></fA64><fA66 i1="01"><s0>FRA</s0></fA66><fC01 i1="01" l="ENG"><s0>Context. IGR J17511-3057 is the second X-ray transient accreting millisecond pulsar discovered by INTEGRAL. It was in outburst for about a month beginning on September 13, 2009. Aims. We analyze the spectral and timing properties of the object and the characteristics of X-ray bursts with the aim to constrain the physical processes responsible for the X-ray production in this class of sources. Methods. We studied the broad-band spectrum of the persistent emission in the 0.8-300 keV energy band using simultaneous INTEGRAL, RXTE and Swift data obtained in September 2009. We also describe the timing properties in the 2-120 keV energy range such as the outburst light curve, pulse profile, pulsed fraction, pulsed emission, and time lags, and moreover study the properties of X-ray bursts discovered by RXTE and INTEGRAL and the recurrence time. Results. The broad-band average spectrum is well described by thermal Comptonization with an electron temperature of kT<sub>e</sub> ∼ 25 keV, soft seed photons of kT<sub>bb</sub> ∼ 0.6 keV, and Thomson optical depth τ<sub>T</sub> ∼ 2 in a slab geometry. During the outburst the spectrum stays remarkably stable with plasma and soft seed photon temperatures and scattering optical depth being constant within errors. We fitted the outburst profile with the exponential model, and using the disk instability model we inferred the outer disk radius to be (4.8-5.4) x 10<sup>10</sup> cm. The INTEGRAL and RXTE data reveal the X-ray pulsation at a period of 4.08 milliseconds up to ∼120 keV. The pulsed fraction is shown to decrease from ∼22% at 3 keV to a constant pulsed fraction of ∼17-18% between 7-30 keV, and then to decrease again to ∼13% at 60 keV. The nearly sinusoidal pulses show soft lags that monotonically increase with energy to about 0.2 ms at 10-20 keV similar to those observed in other accreting pulsars. The short burst profiles indicate hydrogen-poor material at ignition, which suggests either that the accreted material is hydrogen-deficient, or that the CNO metallicity is up to a factor of 2 times solar. However, the variation of the burst recurrence time as a function of m (inferred from the X-ray flux) is much smaller than predicted by helium-ignition models.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="X" l="FRE"><s0>Propriété spectrale</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="ENG"><s0>Spectral properties</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="SPA"><s0>Propiedad espectral</s0><s5>26</s5></fC03><fC03 i1="02" i2="3" l="FRE"><s0>Timing</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Timing</s0><s5>27</s5></fC03><fC03 i1="03" i2="X" l="FRE"><s0>Pulsar RX</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="ENG"><s0>X ray pulsar</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="SPA"><s0>Pulsar RX</s0><s5>28</s5></fC03><fC03 i1="04" i2="X" l="FRE"><s0>Source RX transitoire</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="ENG"><s0>Transient X ray source</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="SPA"><s0>Fuente RX transitoria</s0><s5>29</s5></fC03><fC03 i1="05" i2="X" l="FRE"><s0>Pulsar milliseconde</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="ENG"><s0>Millisecond pulsar</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="SPA"><s0>Pulsar milisegundo</s0><s5>30</s5></fC03><fC03 i1="06" i2="X" l="FRE"><s0>Sursaut RX</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="ENG"><s0>X ray burst</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="SPA"><s0>Arrebato RX</s0><s5>31</s5></fC03><fC03 i1="07" i2="3" l="FRE"><s0>Domaine énergie keV</s0><s5>32</s5></fC03><fC03 i1="07" i2="3" l="ENG"><s0>keV range</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Courbe lumière</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Light curves</s0><s5>33</s5></fC03><fC03 i1="09" i2="X" l="FRE"><s0>Forme impulsion</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="ENG"><s0>Pulse shape</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="SPA"><s0>Forma impulsión</s0><s5>34</s5></fC03><fC03 i1="10" i2="3" l="FRE"><s0>Température électron</s0><s5>35</s5></fC03><fC03 i1="10" i2="3" l="ENG"><s0>Electron temperature</s0><s5>35</s5></fC03><fC03 i1="11" i2="X" l="FRE"><s0>Epaisseur optique</s0><s5>36</s5></fC03><fC03 i1="11" i2="X" l="ENG"><s0>Optical thickness</s0><s5>36</s5></fC03><fC03 i1="11" i2="X" l="SPA"><s0>Espesor óptico</s0><s5>36</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Plasma</s0><s5>37</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>Plasma</s0><s5>37</s5></fC03><fC03 i1="13" i2="3" l="FRE"><s0>Température photon</s0><s5>38</s5></fC03><fC03 i1="13" i2="3" l="ENG"><s0>Photon temperature</s0><s5>38</s5></fC03><fC03 i1="14" i2="X" l="FRE"><s0>Diffusion optique</s0><s5>39</s5></fC03><fC03 i1="14" i2="X" l="ENG"><s0>Optical scattering</s0><s5>39</s5></fC03><fC03 i1="14" i2="X" l="SPA"><s0>Difusión óptica</s0><s5>39</s5></fC03><fC03 i1="15" i2="X" l="FRE"><s0>Modèle</s0><s5>40</s5></fC03><fC03 i1="15" i2="X" l="ENG"><s0>Models</s0><s5>40</s5></fC03><fC03 i1="15" i2="X" l="SPA"><s0>Modelo</s0><s5>40</s5></fC03><fC03 i1="16" i2="3" l="FRE"><s0>Instabilité</s0><s5>41</s5></fC03><fC03 i1="16" i2="3" l="ENG"><s0>Instability</s0><s5>41</s5></fC03><fC03 i1="17" i2="X" l="FRE"><s0>Pulsation RX</s0><s5>42</s5></fC03><fC03 i1="17" i2="X" l="ENG"><s0>X ray pulsation</s0><s5>42</s5></fC03><fC03 i1="17" i2="X" l="SPA"><s0>Pulsación rayos X</s0><s5>42</s5></fC03><fC03 i1="18" i2="X" l="FRE"><s0>Métallicité</s0><s5>43</s5></fC03><fC03 i1="18" i2="X" l="ENG"><s0>Metallicity</s0><s5>43</s5></fC03><fC03 i1="18" i2="X" l="SPA"><s0>Metalicidad</s0><s5>43</s5></fC03><fC03 i1="19" i2="3" l="FRE"><s0>Etoile neutron</s0><s5>44</s5></fC03><fC03 i1="19" i2="3" l="ENG"><s0>Neutron stars</s0><s5>44</s5></fC03><fC03 i1="20" i2="3" l="FRE"><s0>Binaire RX</s0><s5>45</s5></fC03><fC03 i1="20" i2="3" l="ENG"><s0>X-ray binary stars</s0><s5>45</s5></fC03><fC03 i1="21" i2="X" l="FRE"><s0>Source RX binaire</s0><s5>46</s5></fC03><fC03 i1="21" i2="X" l="ENG"><s0>Binary X ray source</s0><s5>46</s5></fC03><fC03 i1="21" i2="X" l="SPA"><s0>Fuente RX binaria</s0><s5>46</s5></fC03><fC03 i1="22" i2="3" l="FRE"><s0>Source RX cosmique</s0><s5>47</s5></fC03><fC03 i1="22" i2="3" l="ENG"><s0>Cosmic x-ray sources</s0><s5>47</s5></fC03><fN21><s1>213</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard></inist></record>Pour manipuler ce document sous Unix (Dilib)
EXPLOR_STEP=$WICRI_ROOT/Wicri/Asie/explor/AustralieFrV1/Data/PascalFrancis/Curation
HfdSelect -h $EXPLOR_STEP/biblio.hfd -nk 004413 | SxmlIndent | more
Ou
HfdSelect -h $EXPLOR_AREA/Data/PascalFrancis/Curation/biblio.hfd -nk 004413 | SxmlIndent | more
Pour mettre un lien sur cette page dans le réseau Wicri
{{Explor lien
|wiki= Wicri/Asie
|area= AustralieFrV1
|flux= PascalFrancis
|étape= Curation
|type= RBID
|clé= Pascal:11-0310959
|texte= Spectral and timing properties of the accreting X-ray millisecond pulsar IGR J17511-3057
}}
| This area was generated with Dilib version V0.6.33. |  |