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| 1 | Search for pulsations in the LMXB EXO 0748-676显示文摘We present here results from our search for X-ray pulsations of the neutron star in the low mass X-ray binary EXO 0748-676 at a frequency near the burstoscillation frequency of 44.7Hz.Using the observations made with the Proportional Counter Array onboard the Rossi X-ray Timing Explorer,we did not find any pulsations in the frequency band of 44.4Hz to 45.0Hz and obtained a 3σ upper limit of 0.47% on the pulsed fraction for any possible underlying pulsation in this frequency band.We also discuss the importance of EXO 0748-676 as a promising source for the detection of Gravitational Waves. | Chetana Jain Biswajit Paul | 2011 | Research in Astronomy and Astrophysics2011，11，5： | 1 |
| 2 | Physics and astrophysics of strong magnetic field systems with eXTP显示文摘In this paper we present the science potential of the enhanced X-ray Timing and Polarimetry(eXTP) mission for studies of strongly magnetized objects. We will focus on the physics and astrophysics of strongly magnetized objects, namely magnetars, accreting X-ray pulsars, and rotation powered pulsars. We also discuss the science potential of eXTP for QED studies. Developed by an international Consortium led by the Institute of High Energy Physics of the Chinese Academy of Sciences, the eXTP mission is expected to be launched in the mid 2020s. | Andrea Santangelo Silvia Zane Hua Feng RenXin Xu Victor Doroshenko Enrico Bozzo Ilaria Caiazzo Francesco Coti Zelati Paolo Esposito Denis González-Caniulef Jeremy Heyl Daniela Huppenkothen Gianluca Israel ZhaoSheng Li Lin Lin Roberto Mignani Nanda Rea Mauro Orlandini Roberto Taverna Hao Tong Roberto Turolla Cristina Baglio Federico Bernardini Niccolo'Bucciantini Marco Feroci Felix Fürst Ersin G??ü? Can Güngör Long Ji FangJun Lu Antonios Manousakis Sandro Mereghetti Romana Mikusincova Biswajit Paul Chanda Prescod-Weinstein George Younes Andrea Tiengo YuPeng Xu Anna Watts Shu Zhang Shuang-Nan Zhang | 2019 | Science China(Physics,Mechanics & Astronomy)2019，62，2： | 1 |
| 3 | Orbital X-ray modulation study of three supergiant HMXBs显示文摘We present the orbital X-ray modulation study of three high mass X-ray binary systems,IGR J18027-2016,IGR J18483-0311 and IGR J16318-4848,using data obtained with RXTE-ASM,Swift-BAT and INTEGRAL-ISGRI.Using the long term light curves of the eclipsing HMXB IGR J18027-2016,obtained with Swift-BAT in the energy range 15-50keV and INTEGRAL-ISGRI in the energy range 22-40keV,we have determined three new mid eclipse times.The newly determined mid eclipse times together with the known values were used to derive an accurate value of the orbital period of 4.5693(4) d at MJD 52168 and an upper limit of 3.9(1.2) ×10-7 d d-1 on the period derivative.We have also accurately determined an orbital period of 18.5482(88) d for the intermediate system IGR J18483-0311,which displays an unusual behavior and shares many properties with the known SFXTs and persistent supergiant systems.This is a transient source and the outbursts occur intermittently at intervals of 18.55d.Similarly,in the third supergiant system,IGR J16318-4848,we have found that the outbursts are separated by intervals of 80 d or its multiples,suggesting a possible orbital period. | Chetana Jain Biswajit Paul Anjan Dutta | 2009 | Research in Astronomy and Astrophysics2009，9，12： | 0 |
| 4 | Variations in the X-ray eclipse transitions of Cen X-3显示文摘We report here an investigation of the X-ray eclipse transitions of the high mass X-ray binary pulsar Cen X-3 in different intensity states.The long term light curve of Cen X-3 obtained with RXTE-ASM spanning more than 5000d shows strong aperiodic flux variations with low and high states.We have investigated the eclipse transitions of Cen X-3 in different intensity states with data obtained from pointed observations with the more sensitive instruments onboard ASCA,BeppoSAX,XMMNewton,Chandra and RXTE.We found a very clear trend of sharp eclipse transitions in the high state and longer transitions in the low state.This is a confirmation of this feature first observed with the RXTE-ASM but now observed with much better clarity.From the light curves obtained from several missions,it is seen that the eclipse egress in the low state starts earlier by an orbital phase of 0.02 compared to the eclipse egress in the high state indicating that the observed X-rays originate from a much larger region.We have also performed spectral analysis of the post-eclipse part of each observation.From BeppoSAX observations,the out-of-eclipse X-ray flux is found to differ by a factor of ~26 during the high and low intensity states while the eclipse count rates differ by a factor of only ~ 4.7.This indicates that in the low state,there is an additional scattering medium which scatters some of the source photons towards the observer even when the neutron star is completely eclipsed.We could also resolve the three iron line components using XMM-Newton observation in the low state.By comparing the iron line equivalent width during the high and low states,it is seen that the width of the iron line is relatively large during the low state which supports the fact that significant reprocessing and scattering of X-rays takes place in the low state. | Jincy Devasia Biswajit Paul Marykutty James Kavila Indulekha | 2010 | Research in Astronomy and Astrophysics2010，10，11： | 0 |
| 5 | Observatory science with eXTP显示文摘In this White Paper we present the potential of the enhanced X-ray Timing and Polarimetry(eXTP) mission for studies related to Observatory Science targets. These include flaring stars, supernova remnants, accreting white dwarfs, low and high mass X-ray binaries, radio quiet and radio loud active galactic nuclei, tidal disruption events, and gamma-ray bursts. eXTP will be excellently suited to study one common aspect of these objects: their often transient nature. Developed by an international Consortium led by the Institute of High Energy Physics of the Chinese Academy of Science, the eXTP mission is expected to be launched in the mid 2020s. | Jean J.M.in 't Zand Enrico Bozzo JinLu Qu Xiang-Dong Li Lorenzo Amati Yang Chen Immacolata Donnarumma Victor Doroshenko Stephen A.Drake Margarita Hernanz Peter A.Jenke Thomas J.Maccarone Simin Mahmoodifar Domitilla de Martino Alessandra De Rosa Elena M.Rossi Antonia Rowlinson Gloria Sala Giulia Stratta Thomas M.Tauris Joern Wilms XueFeng Wu Ping Zhou Iván Agudo Diego Altamirano Jean-Luc Atteia Nils A.andersson M.Cristina Baglio David R.Ballantyne Altan Baykal Ehud Behar Tomaso Belloni Sudip Bhattacharyya Stefano Bianchi Anna Bilous Pere Blay Joao Braga Sφren Brandt Edward F.Brown Niccolo Bucciantini Luciano Burderi Edward M.Cackett Riccardo Campana Sergio Campana Piergiorgio Casella Yuri Cavecchi Frank Chambers Liang Chen Yu-Peng Chen Jér?me Chenevez Maria Chernyakova ChiChuan Jin Riccardo Ciolfi Elisa Costantini Andrew Cumming Antonino D'Aì Zi-Gao Dai Filippo D'Ammando Massimiliano De Pasquale Nathalie Degenaar Melania Del Santo Valerio D'Elia Tiziana Di Salvo Gerry Doyle Maurizio Falanga XiLong Fan Robert D.Ferdman Marco Feroci Federico Fraschetti Duncan K.Galloway Angelo F.Gambino Poshak Gandhi MingYu Ge Bruce Gendre Ramandeep Gill Diego G?tz Christian Gouiffès Paola Grandi Jonathan Granot Manuel Güdel Alexander Heger Craig O.Heinke Jeroen Homan Rosario Iaria Kazushi Iwasawa Luca Izzo Long Ji Peter G.Jonker Jordi José Jelle S.Kaastra Emrah Kalemci Oleg Kargaltsev Nobuyuki Kawai Laurens Keek Stefanie Komossa Ingo Kreykenbohm Lucien Kuiper Devaky Kunneriath Gang Li En-Wei Liang Manuel Linares Francesco Longo FangJun Lu Alexander A.Lutovinov Denys Malyshev Julien Malzac Antonios Manousakis Ian McHardy Missagh Mehdipour YunPeng Men Mariano Méndez Roberto P.Mignani Romana Mikusincova M.Coleman Miller Giovanni Miniutti Christian Motch Joonas Nättilä Emanuele Nardini Torsten Neubert Paul T.O'Brien Mauro Orlandini Julian P.Osborne Luigi Pacciani Stéphane Paltani Maurizio Paolillo Iossif E.Papadakis Biswajit Paul Alberto Pellizzoni Uria Peretz Miguel A.Pérez Torres Emanuele Perinati Chanda Prescod-Weinstein Pablo Reig Alessandro Riggio Jerome Rodriguez Pablo Rodríguez-Gil Patrizia Romano Agata Rózańska Takanori Sakamoto Tuomo Salmi Ruben Salvaterra andrea Sanna andrea Santangelo Tuomas Savolainen Stéphane Schanne Hendrik Schatz LiJing Shao andy Shearer Steven N.Shore Ben W.Stappers Tod E.Strohmayer Valery F.Suleimanov Jirí Svoboda F.-K.Thielemann Francesco Tombesi Diego F.Torres Eleonora Torresi Sara Turriziani andrea Vacchi Stefano Vercellone Jacco Vink Jian-Min Wang JunFeng Wang Anna L.Watts ShanShan Weng Nevin N.Weinberg Peter J.Wheatley Rudy Wijnands Tyrone E.Woods Stan E.Woosley ShaoLin Xiong YuPeng Xu Zhen Yan George Younes WenFei Yu Feng Yuan Luca Zampieri Silvia Zane andrzej A.Zdziarski Shuang-Nan Zhang Shu Zhang Shuo Zhang Xiao Zhang Michael Zingale | 2019 | Science China(Physics,Mechanics & Astronomy)2019，62，2： | 0 |
| 6 | Variations of the harmonic components of the X-ray pulse profile of PSR B1509–58显示文摘We used the Fourier decomposition technique to investigate the stability of the X-ray pulse profile of a young pulsar PSR B1509–58 by studying the relative amplitudes and phase differences of its harmonic components with respect to the fundamental using data from the Rossi X-Ray Timing Explorer. Like most young rotation powered pulsars, PSR B1509–58 has a high spin down rate. It also has less timing noise, allowing accurate measurement of higher order frequency derivatives which in turn helps in the study of the physics of pulsar spin down. Detailed investigation of pulse profiles over the years will help us establish any possible connection between the timing characteristics and the high energy emission characteristics for this pulsar.Furthermore, the study of pulse profiles of short period X-ray pulsars can also be useful when used as a means of interplanetary navigation. The X-ray pulse profile of this source has been analyzed for 15 yr(1996–2011). The long term average amplitudes of the first, second and third harmonics(and their standard deviation for individual measurements) compared to the fundamental are 36.9%(1.7%), 13.4%(1.9%) and 9.4%(1.8%) respectively. Similarly, the phases of the three harmonics(and standard deviations) with respect to the fundamental are 0.36(0.06), 1.5(0.2) and 2.5(0.3) radian respectively. We do not find any significant variation of the harmonic components of the pulse profile in comparison to the fundamental. | Pragati Pradhan Biswajit Paul Harsha Raichur Bikash Chandra Paul | 2015 | Research in Astronomy and Astrophysics2015，15，1： | 0 |
| 7 | Pulse profile stability of the Crab pulsar显示文摘We present an X-ray timing analysis of the Crab pulsar, PSR B0531+21, using archival RXTE data. We have investigated the stability of the Crab pulse profile, in soft (2-20 keV) and hard (30-100 keV) X-ray energies, over the last decade of RXTE operation. The analysis includes measurement of the separation between the two pulse peaks and the intensity and widths of the two peaks. We did not find any significant time dependency in the pulse shape. The two peaks have been stable in phase, intensity and width for the last ten years. The first pulse is relatively stronger at soft X-rays. The first pulse peak is narrower than the second peak in both soft and hard X-ray energies. Both the peaks show a slow rise and a steeper fall. The ratio of the pulsed photons in the two peaks is also constant in time. | Chetana Jain Biswajit Paul | 2011 | Research in Astronomy and Astrophysics2011，11，10： | 0 |
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