Chenevez, Jérôme

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Downloaded from orbit.dtu.dk on: Dec 19, 2017INTEGRAL observations of long X-ray burstsChenevez, JérômePublication date:2011Document VersionPublisher's PDF, also known as Version of recordLink back to DTU OrbitCitation (APA):Chenevez, J. (2011). INTEGRAL observations of long X-ray bursts [Sound/Visual production (digital)].International Conference Physics of Neutron Stars, St. Petersburg, Russian Federation, 11/07/2011,http://www.ioffe.ru/astro/NS2011Jérôme ChenevezINTEGRAL observations of long X-ray burstsNS-11, St. PetersburgJuly 14, 2011Jérôme ChenevezINTEGRAL observations of long X-ray burstsMaurizio FalangaErik KuulkersSøren BrandtNiels LundAndrew CummingHendrik Schatz Duncan GallowayTim OosterbroekNS-11, St. PetersburgJuly 14, 2011Jérôme Chenevez, DTU Space, Technical University of DenmarkNS-11, St. PetersburgJuly 14, 2011 INTEGRAL long burstsShort burstsMore or less long bursts Current investigations of the various types of thermonuclear bursts aim to draw a consistent picture of the ignition and burning processes in relation with the accretion regime of the neutron stars.Distribution of all (MINBAR*) X-ray bursts as a function of their exponential decay time*Multi-Instrument Burst Archivein collaboration with D. Galloway, J. in ‘t Zand, et al.MOTIVATIONJérôme Chenevez, DTU Space, Technical University of DenmarkNS-11, St. PetersburgJuly 14, 2011 INTEGRAL long burstsShort bursts≈5000More or less long burstsMOTIVATIONOrdinary He burstsH/He bursts Unusual long* burstsSuperbursts17* 19*Intermediate long bursts:duration > 12 minFrom 14 sourcesFrom 11 sources*Multi-Instrument Burst Archivein collaboration with D. Galloway, J. in ‘t Zand, et al.Distribution of all (MINBAR*) X-ray bursts as a function of their exponential decay timeJérôme Chenevez, DTU Space, Technical University of DenmarkNS-11, St. PetersburgJuly 14, 2011 INTEGRAL long burstsINTEGRALJEM-X :100 cm2 @ 10 keV3-25 keVFoV: 5º,   3’ reso.IBIS :1000 cm2 @ 20 keV18 keV – 10 MeVFoV ≈ 12ºSPI :20 keV – 8 MeV2.2 keV @ 1.3 MeVFoV ≈ 15ºJérôme Chenevez, DTU Space, Technical University of DenmarkNS-11, St. PetersburgJuly 14, 2011 INTEGRAL long bursts2˚NGPThe Galactic Center region as seen by JEM-XJérôme Chenevez, DTU Space, Technical University of DenmarkNS-11, St. PetersburgJuly 14, 2011 INTEGRAL long bursts2˚NGPThe Galactic Center region as seen by JEM-X94 X-ray bursters known to date; ≈2/3 located in the Galactic Bulge regionJérôme Chenevez, DTU Space, Technical University of DenmarkNS-11, St. PetersburgJuly 14, 2011 INTEGRAL long bursts2465 2465.5 2466 2466.550100150TIME (d)RATE (count/s)KP484_DETE_LC30sIGR J17254−3257|||||Example of burst detections in JEM-X detector light curveKP-484, Oct. 2006(30s bins)Jérôme Chenevez, DTU Space, Technical University of DenmarkNS-11, St. PetersburgJuly 14, 2011 INTEGRAL long bursts2465.26 2465.27 2465.28 2465.29 2465.3 2465.31 2465.3215202530354045TIME (d)RATE (count/s)KP484_DETE_LC30s   ScWs 41−43  [3−10 keV]IGR J17254−3257GX 354−0ScW 41 |||ScW 42 |  ScW 43||← slew!Long burst from IGR J17254-32571st October 2006Jérôme Chenevez, DTU Space, Technical University of DenmarkNS-11, St. PetersburgJuly 14, 2011 INTEGRAL long bursts2465.26 2465.27 2465.28 2465.29 2465.3 2465.31 2465.3215202530354045TIME (d)RATE (count/s)KP484_DETE_LC30s   ScWs 41−43  [3−10 keV]IGR J17254−3257GX 354−0ScW 41 |||ScW 42 |  ScW 43||← slew!(Burst 2)Chenevez et al., 2007Long burst from IGR J17254-32571st October 2006Jérôme Chenevez, DTU Space, Technical University of DenmarkNS-11, St. PetersburgJuly 14, 2011 INTEGRAL long burstsDifferent lasting bursts from IGR J17254- 3257 can be explained by a transition between two slightly different accretion rates. The short event is a mixed H/He burst triggered by a weak H flash, while the long burst is the result of the burning of a large He pile produced by steady H burning at a slightly higher accretion rate.17 February 20041 October 2006Long burst from IGR J17254-32575s bins20s binsJérôme Chenevez, DTU Space, Technical University of DenmarkNS-11, St. PetersburgJuly 14, 2011 INTEGRAL long burstsMarch 2004 April 2005 April 2007SLX 1737-282 3/4 bursts in INTEGRAL; all intermediate long!(Falanga, Chenevez, et al., 2008)10s bin light-curvesJérôme Chenevez, DTU Space, Technical University of DenmarkNS-11, St. PetersburgJuly 14, 2011 INTEGRAL long burstsSLX 1737-282 Time-resolved spectral analysesMarch 2004 April 2005 April 2007Jérôme Chenevez, DTU Space, Technical University of DenmarkNS-11, St. PetersburgJuly 14, 2011 INTEGRAL long burstsSLX 1737-282 Time-resolved spectral analysesMarch 2004 April 2005 April 2007LEddThe time resolved spectral analysis reveals variations in the temperature and inferred blackbody radius that are consistent with expansion and contraction of the neutron star photosphere.The luminosity reaches the Eddington limit, allowing us to derive the distance to the source: d  7.5 kpcJérôme Chenevez, DTU Space, Technical University of DenmarkNS-11, St. PetersburgJuly 14, 2011 INTEGRAL long bursts(2005)JEM-XLong riseSoft precursorLarge radius expansionfollowed by contraction.Progressive hardening15 September  2003SLX 1735-269 The first long burst detected by INTEGRAL1st interpretation was mix burning of H/He (Molkov et al. (2005). In ‘t Zand et al. (2007) classified the source as UCXB candidate. Pure He burning.Jérôme Chenevez, DTU Space, Technical University of DenmarkNS-11, St. PetersburgJuly 14, 2011 INTEGRAL long burstsTwo phase long burst from GX 3+1The peculiar long burst from GX 3+1 on August 31, 2004(Chenevez et al., 2006)Jérôme Chenevez, DTU Space, Technical University of DenmarkNS-11, St. PetersburgJuly 14, 2011 INTEGRAL long burstsTwo phase long burst from GX 3+1He flashH/He tail ?Two-phases burst (Chenevez et al., 2006)The peculiar long burst from GX 3+1 on August 31, 2004Jérôme Chenevez, DTU Space, Technical University of DenmarkNS-11, St. PetersburgJuly 14, 2011 INTEGRAL long burstsRelation with accretion rateLong term persistent flux of GX 3+1Superburst(Kuulkers, 2002)long burst31/08-2004RXTE/ASMAn aborted superburst due to the premature ignition of a carbon layer triggered by an He detonation could also be considered.The peculiar long burst from GX 3+1 on August 31, 2004(Chenevez et al., 2006)Jérôme Chenevez, DTU Space, Technical University of DenmarkNS-11, St. PetersburgJuly 14, 2011 INTEGRAL long burstsSUMMARYSource Date Tb (s) |  (s) Eb (erg) Acc. Rate*(g/cm2/s) Burning Reference GX 3+1 20040831 1800 | 131 2 1040 10 000 He / H Chenevez et al., 2006 IGR J17254-3257  20061001   900 | 216 2 1040  400  (H)He  Chenevez et al., 2007  SLX 1737-282 2004030920050411200704021500 | 2751800 | 323~900 | 2810.7 10411.2 10411.0 1041  800 He He He Falanga, Chenevez  et al., 2008 SLX 1735-269 20030915 2000 | 400 2 1041 1 500 H? Molkov et al., 2005   Intermediate long X-ray bursts observed with INTEGRAL*Eddington mass accretion rate per unit area: 12-5  cm g10   smEddThe monitoring of long X-ray bursts with INTEGRAL/JEM-X has led to the discovery of six intermediate bursts longer than ≈15 minutes: ⅓ of the total population, and ½ of the bursts, which occurred in the same period.(UCXB: in ‘t Zand et al, 2007)eJérôme Chenevez, DTU Space, Technical University of DenmarkNS-11, St. PetersburgJuly 14, 2011 INTEGRAL long burstsSAX J1747.0-2853 (Chenevez et al., 2011)Precursor  →LC (3-25 keV)reaches Eddington ⇒ PRE  d9kpcMAXI→To-date last observed superburst SAX J1753.0-2853 on February 13thChenevez et al., in prep.The superburst peak reaches similar count-rate as previous PRE bursts from this source, and is consistent with a shock-triggered He flash precursor as seen in other superbursts (Weinberg & Bildsten, 2007).Chenevez et al., ATel 3183Jérôme Chenevez, DTU Space, Technical University of DenmarkNS-11, St. PetersburgJuly 14, 2011 INTEGRAL long burstsSAX J1747.0-2853 (Chenevez et al., 2011)Intermediatelong burst!To-date last observed superburst SAX J1753.0-2853 on February 13thChenevez et al., in prep.Precursor  →Jérôme Chenevez, DTU Space, Technical University of DenmarkNS-11, St. PetersburgJuly 14, 2011 INTEGRAL long burstsAn exceptional sequence of events:1. ATel 3162 : “Fermi LAT detection of an outburst from the Galactic center region“≈20s GeV burst 3 days prior to the superburst.2. ATel 3163 : “Swift/XRT detects SAX J1747.0-2853 in outburst”Associates this source with the origin of the LAT burst.3a. ATel 3172* : “INTEGRAL sees continuing activity from SAX J1747.0-2853”Reports only on strong X-ray flaring activity!3b. ATel 3183* : “First superburst observed by INTEGRAL, from SAX J1747.0-2853”Superburst preceded by an intermediately long burst.4. ATel 3217 : “SAX J1747.0-2853: 'normal' thermonuclear bursts resumed”Burst quenching time upper limit of 25 days (as expected).To-date last observed superburst SAX J1753.0-2853 on February 13thJérôme Chenevez, DTU Space, Technical University of DenmarkNS-11, St. PetersburgJuly 14, 2011 INTEGRAL long burstsSummary• First superburst observed from SAX J1753.0-2853 – early in outburst• 2nd superburst so far from a (normal) X-ray transient (4U1608-52 in 2005)• 2nd shorter quenching time (4U 0614+09 : 19 days)• Photospheric Radius Expansion (TBC)• Peculiar start of the outburst with a GeV event• First observation of a firestarter (right heating / C supply conditions?)  • Need theoretical explanation from numerical simulationsTo-date last observed superburst SAX J1753.0-2853 on February 13thJérôme Chenevez, DTU Space, Technical University of DenmarkNS-11, St. PetersburgJuly 14, 2011 INTEGRAL long burstsMost intermediate bursts are observed from low luminosity sources and are interpreted as long pure He bursts. If no H is accreted, they are consistent with the burning of a slowly accreted, thick He layer, in Ultra Compact X-ray Binaries (UCXB) where the donor star is probably a degenerated helium white dwarf.Of special interest are bursters showing events with very different durations, thus allowing us to study transitions between different nuclear burning regimes.Depending on the actual accretion rate, either the burning of a large amount of H-rich material is triggered by an He flash, or a thick sedimented column of He is triggered by weak H ignition.Relation with superbursts…?CONCLUSIONS

INTEGRAL observations of long X-ray bursts

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INTEGRAL observations of long X-ray bursts

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