159 articles – 2000 Notices  [english version]
HAL : in2p3-00712215, version 1

Fiche concise  Récupérer au format
Characterization of new hard X-ray cataclysmic variables
Bernardini F., de Martino D., Falanga M., Mukai K., Matt G. et al
Astronomy and Astrophysics 542 (2012) 22 - http://hal.in2p3.fr/in2p3-00712215
Planète et Univers/Astrophysique/Astrophysique stellaire et solaire
Physique/Astrophysique/Astrophysique stellaire et solaire
Characterization of new hard X-ray cataclysmic variables
F. Bernardini, D. de Martino, M. Falanga, K. Mukai, G. Matt, J.-M. Bonnet-Bidaud1, N. Masetti, M. Mouchet2, 3
1 :  SAp - Service d'Astrophysique
http://www-dapniai2.cea.fr/Dapnia/Sap/Fr/homepage.php
CEA : DSM/IRFU
Service d'Astrophysique, CEA-Saclay, DSM/DAPNIA/SAp, Bât. 709, L'Orme des Merisiers, F-91 191 Gif-sur-Yvette Cedex, France
France
2 :  APC - UMR 7164 - AstroParticule et Cosmologie
http://www.apc.univ-paris7.fr/
CNRS : UMR7164 – IN2P3 – Observatoire de Paris – Université Paris VII - Paris Diderot – CEA : DSM/IRFU
APC - UMR 7164, Université Paris Diderot, 10 rue Alice Domon et Léonie Duquet, case postale 7020, F-75205 Paris Cedex 13
France
3 :  LUTH - Laboratoire Univers et Théories
http://luth.obspm.fr/
CNRS : UMR8102 – INSU – Observatoire de Paris – Université Paris VII - Paris Diderot
5 place Jules Janssen 92195 Meudon cedex
France
APC - Cosmologie et gravitation
Aims: We aim at characterizing a sample of nine new hard X-ray selected cataclysmic variable (CVs), to unambiguously identify them as magnetic systems of the intermediate polar (IP) type. Methods: We performed detailed timing and spectral analysis by using X-ray, and simultaneous UV and optical data collected by XMM-Newton, complemented with hard X-ray data provided by INTEGRAL and Swift. The pulse arrival time were used to estimate the orbital periods. The broad band X-ray spectra were fitted using composite models consisting of different absorbing columns and emission components. Results: Strong X-ray pulses at the white dwarf (WD) spin period are detected and found to decrease with energy. Most sources are spin-dominated systems in the X-rays, though four are beat dominated at optical wavelengths. We estimated the orbital period in all system (except for IGR J16500-3307), providing the first estimate for IGR J08390-4833, IGR J18308-1232, and IGR J18173-2509. All X-ray spectra are multi-temperature. V2069 Cyg and RX J0636+3535 posses a soft X-ray optically thick component at kT ~ 80 eV. An intense Kα Fe line at 6.4 keV is detected in all sources. An absorption edge at 0.76 keV from OVII is detected in IGR J08390-4833. The WD masses and lower limits to the accretion rates are also estimated. Conclusions: We found all sources to be IPs. IGR J08390-4833, V2069 Cyg, and IGR J16500-3307 are pure disc accretors, while IGR J18308-1232, IGR J1509-6649, IGR J17195-4100, and RX J0636+3535 display a disc-overflow accretion mode. All sources show a temperature gradient in the post-shock regions and a highly absorbed emission from material located in the pre-shock flow which is also responsible for the X-ray pulsations. Reflection at the WD surface is likely the origin of the fluorescent iron line. There is an increasing evidence for the presence of a warm absorber in IPs, a feature that needs future exploration. The addition of two systems to the subgroup of soft X-ray IPs confirms a relatively large (~30%) incidence. Based on observations obtained with XMM-Newton and INTEGRAL, ESA science missions with instruments and contributions directly funded by ESA Member States; and Swift, a NASA science mission with Italian participation.

Articles dans des revues avec comité de lecture
06/2012
Astronomy and Astrophysics (Astron. Astrophys.)
Publisher EDP Sciences
ISSN 0004-6361 (eISSN : 1432-0756)
542
22

binaries: close – X-rays: binaries – accretion – accretion disks – novae – cataclysmic variables
Lien vers le texte intégral : 
http://fr.arXiv.org/abs/1204.3758