# 2011A&A...531A.130B

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 Query : 2011A&A...531A.130B

2011A&A...531A.130B - Astronomy and Astrophysics, volume 531A, 130-130 (2011/7-1)

XMM-Newton observations of IGR J18410-0535: the ingestion of a clump by a supergiant fast X-ray transient.

BOZZO E., GIUNTA A., CUSUMANO G., FERRIGNO C., WALTER R., CAMPANA S., FALANGA M., ISRAEL G. and STELLA L.

Abstract (from CDS):

IGRJ18410-0535 is a supergiant fast X-ray transients. This subclass of supergiant X-ray binaries typically undergoes few-hour-long outbursts reaching luminosities of 1036-1037 erg/s, the occurrence of which has been ascribed to the combined effect of the intense magnetic field and rotation of the compact object hosted in them and/or the presence of dense structures (clumps'') in the wind of their supergiant companion. IGRJ18410-0535 was observed for 45ks by XMM-Newton as part of a program designed to study the quiescent emission of supergiant fast X-ray transients and clarify the origin of their peculiar X-ray variability. We carried out an in-depth spectral and timing analysis of these XMM-Newton data. IGRJ18410-0535 underwent a bright X-ray flare that started about 5ks after the beginning of the observation and lasted for ∼15ks. Thanks to the capabilities of the instruments on-board XMM-Newton, the whole event could be followed in great detail. The results of our analysis provide strong convincing evidence that the flare was produced by the accretion of matter from a massive clump onto the compact object hosted in this system. By assuming that the clump is spherical and moves at the same velocity as the homogeneous stellar wind, we estimate a mass and radius of Mcl≃1.4x1022g and Rcl≃8x1011cm. These are in qualitative agreement with values expected from theoretical calculations. We found no evidence of pulsations at ∼4.7s after investigating coherent modulations in the range 3.5ms-100s. A reanalysis of the archival ASCA and Swift data of IGRJ18410-0535, for which these pulsations were previously detected, revealed that they were likely to be due to a statistical fluctuation and an instrumental effect, respectively.

Journal keyword(s): X-rays: binaries - stars: individual: IGR J18410-0535 - stars: neutron - X-rays: stars

Full paper

 Number of rows : 11
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 HD 74194 HXB 08 40 47.7915253032 -45 03 30.235569624 7.05 7.77 7.55 8.70   O8.5Ib-II(f)p 189 0
2 HD 306414 s*b 11 21 46.8238550520 -59 51 47.970396396 10.12 10.69 10.23 10.00   B1Ia 143 0
3 2MASS J16463526-4507045 HXB 16 46 35.2590465192 -45 07 04.609890912   15.2       O9.5Ia 89 1
4 2MASS J16480656-4512068 HXB 16 48 06.56 -45 12 06.8           O8.5Iab 126 2
5 AX J1739.1-3020 HXB 17 39 11.5515537336 -30 20 37.787917704     14.40 13.91   O8.5Iab(f) 148 1
6 IGR J17544-2619 HXB 17 54 25.2722906112 -26 19 52.576928292   14.71 12.94 12.10 10.38 O9Ib 170 0
7 3EG J1837-0423 Rad 18 38 52.0 -04 16 16           ~ 83 1
8 SNR G026.6-00.1 SR? 18 40 -05.7           ~ 15 0
9 [KRL2007b] 332 HXB 18 41 00.43 -05 35 46.5           B1Ib 120 1
10 IGR J18483-0311 HXB 18 48 17.2064716656 -03 10 16.865225040 23.702 25.162 21.884 17.888 15.88 B0.5Ia 115 0
11 NAME Scutum Spiral Arm PoG ~ ~           ~ 316 0

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2022.08.14-08:43:10