On the formation of the peculiar LMXB IGR J in Terzan 5

Slides:

Advertisements

Similar presentations

Magnetars in Supernova Remnants & Magnetar Formation Jacco Vink Isolated NSs, London, April, 2006 Magnetars in Supernova Remnants & Magnetar Formation.

Advertisements

X-ray pulsars in wind-fed accretion systems 王伟 (NAOC) July 2009, Pulsar Summer School Beijing.

Accretion in Binaries Two paths for accretion –Roche-lobe overflow –Wind-fed accretion Classes of X-ray binaries –Low-mass (BH and NS) –High-mass (BH and.

AS 3004 Stellar Dynamics Mass transfer in binary systems Mass transfer occurs when –star expands to fill Roche-lobe –due to stellar evolution –orbit, and.

Neutron Stars Chandrasekhar limit on white dwarf mass Supernova explosions –Formation of elements (R, S process) –Neutron stars –Pulsars Formation of X-Ray.

HOW MANY NEUTRON STARS ARE BORN RAPIDLY ROTATING? HOW MANY NEUTRON STARS ARE BORN RAPIDLY ROTATING? NIKOLAOS STERGIOULAS DEPARTMENT OF PHYSICS ARISTOTLE.

Low Mass X-ray Binaries and Accreting Millisecond Pulsars A. Patruno R. Wijnands R. Wijnands M. van der Klis M. van der Klis P. Casella D. Altamirano D.

Magnetars origin and progenitors with enhanced rotation S.B. Popov, M.E. Prokhorov (Sternberg Astronomical Institute) (astro-ph/ )

Mass Loss and Evolution of Low-Mass X-ray Binaries Xiang-Dong Li Department of Astronomy Nanjing University

Pulsars in Low-Mass X-Ray Binaries Deepto Chakrabarty Massachusetts Institute of Technology.

1 Magnetars origin and progenitors with enhanced rotation S.B. Popov, M.E. Prokhorov (Sternberg Astronomical Institute) (astro-ph/ ) Poster N 21.

Galloway, “Accreting neutron star spins and the prospects for GW searches” 1 Accreting neutron star spins and the prospects for GW searches Duncan Galloway.

Two stories from the life of binaries: getting bigger and making magnetars Sergei Popov, Mikhail Prokhorov (SAI MSU) This week SAI celebrates its 175 anniversary.

Spin and Orbital Evolution of the Accreting Millisecond Pulsar SAX J : Implications for Gravitational Wave Searches Deepto Chakrabarty Massachusetts.

Accreting Neutron Stars, Equations of State, and Gravitational Waves C. B. Markwardt NASA/GSFC and U. Maryland.

Neutron star low-mass X-ray binaries Rudy Wijnands Anton Pannekoek Institute for Astronomy University of Amsterdam 3 August 2015Lorentz center, Leiden.

Spin angular momentum evolution of the long-period Algols Dervişoğlu, A.; Tout, Christopher A.; Ibanoğlu, C. arXiv:

Simulation of the Recycled Pulsar Evolution Pan Yuanyue, Wang Na and Zhang Chengmin, Xinjiang Astronomical Observatory, CAS, Urumqi, China National Astronomical.

He star evolutionary channel to intermediate-mass binary pulsars with a short-orbital-period Chen Wen-Cong School of Physics, Peking University Department.

An ultra-massive, fast-spinning white dwarf in a peculiar binary system S. Mereghetti (1), A.Tiengo (1), P. Esposito (1), N. La Palombara (1), G.L.Israel.

1 ACCRETING X-RAY MILLISECOND PULSARS IN OUTBURST M A U R I Z I O F A L A N G A Service d‘Astrophysique, CEA –Saclay Collaborators: J. Poutanen, L. Kuipers,

1 ACCRETING X-RAY MILLISECOND PULSARS M A U R I Z I O F A L A N G A & E R I N W. B O N N I N G NS day, ParisJune 27, 2007 Service d‘Astrophysique, CEA.

Thin accretion discs around millisecond X-ray pulsars —arXiv: v1 Reporter : Shaoyong.

Is Radio−Ejection ubiquitous among Accreting Millisecond Pulsar? Luciano Burderi, University of Cagliari Collaborators: Tiziana di Salvo, Rosario Iaria,

Millisecond Pulsar and kHz QPOs of LMXB Chengmin ZHANG, NAOC 2011 – NAOC Collaborators: J. Wang, L.M. Song, Y.J. Lei, F. Zhang.

Radio Observations of X-ray Binaries : Solitary and Binary Millisecond Pulsars Jeong-Sook Kim 1 & Soon-Wook Kim 2  Department of Space Science and Astronomy.

Populations of accreting X-ray sources in galaxies

A Toy Model for 3:2 HFQPO Pairs in Black Hole Binaries XTE J and GRO J Ding-Xiong WANG( 汪定雄 ), Zhao-Ming GAN (speaker, 甘朝明 ), Chang-Yin.

Spin-up and Spin-down of Accreting Millisecond Pulsars Alessandro Papitto Università di Roma Tor Vergata INAF-Astronomical Observatory of Rome & my research.

Do Old Neutron Stars Shiver to Keep Warm? Jeremy S. Heyl Harvard-Smithsonian CfA.

1 X-ray enhancement and long- term evolution of Swift J arXiv: Authors: O. Benli, S. Caliskan, U. Ertan et al. Reporter: Fu, Lei.

THE PECULIAR EVOLUTIONARY HISTORY OF IGR J IN TERZAN 5 A. Patruno Reporter: Long Jiang ( 姜龙 )

The Radio Millisecond Pulsar PSR J : A Link to Low-Mass X-Ray Binaries Slavko Bogdanov.

Timing Features of XTE J in 2003 March outburst Fan Zhang et al. (astro-ph/ ) --Possible Evidence for Accreting Blobs.

Spin up/down processes of X-ray pulsars arXiv: v1; v2; v1; reporter: Shaoyong

INAF, Osservatorio Astronomico di Roma XI Advanced School of Astrophysics, Brazil, 1-6 September 2002.

Hunting for Glitches Sarah Buchner. …are the leftover cores from supernova explosions. Almost black holes Neutron stars are very dense (10 17 kg/m 3 )

Death of Stars II Physics 113 Goderya Chapter(s): 14

Supercritical Accretion in the Evolution of Neutron Star Binaries and Its Implications Chang-Hwan 1 Nuclear Physics A 928 (2014)

Low frequency observation of both pulsar wind and magnetodipole radiation from switch on-off pulsars Ya.N. Istomin P.N. Lebedev Physical Institute, Moscow,

SAX J : Witnessing the Banquet of a Hidden Black Widow? Luciano Burderi (Dipartimento di Fisica, Universita’ di Cagliari) Tiziana Di Salvo (Dipartimento.

Many facets of Neutron Stars Astrosat and beyond Biswajit Paul Raman Research Institute, Bangalore.

Be/X-Ray 双星中的中子星自传演化成忠群南京大学 Contents 1. Introduction (1) Observed period gap for BeXBs (2) Possible interpretation by the authors 2. What.

Formation of Redback and Black Widow Binary Millisecond Pulsars

Binary Origin of Blue Stragglers Xuefei CHEN Yunnan Observatory, CHINA.

kHz QPOs of LMXBs Constrains on Pulsar Parameters Chengmin Zhang & Hongxing Yin National Astronomical Observatories, Beijing.

Recent Progress about kHz QPO and Spin in LMXB and their implications C.M. Zhang, H.X. Yin, Y. Yan, L.M. Song, F. Zhang National Astronomical Observatories,

Constraining the Equation Of State (EOS) of neutron stars with eXTP/GDP Long Ji.

Black Widow Pulsars(BWP): the Price of Promiscuity A. R. King, M. B. Davies and M. E. Beer, 2003,MNRAS,345,678 Fu Lei

Eccentric Binary Millisecond Pulsars Paulo C. C. Freire arXiv: v1.

Tobias Jogler Max-Planck Institut für Physik IMPRS YSW Ringberg 2007 VHE emission from binary systems Outline Binary systems Microquasar Pulsar binaries.

A pulsar is a supernova remnant which is a super dense, rapidly spinning neutron star which emits dipole electromagnetic radiation and features a strong.

Gravitational Waves What are they? How can they be detected?

Searching for accreting neutron stars

Magnetic Dipoles and Angular Momenta

Neutron Stars and Black Holes

Towards a more perfect wind braking model

Basic Properties By Dr. Lohse, University of Berlin

Progenitors of long GRBs

Probing Neutron Star interiors with ET ?

Magnetar SGR By Christina Balanduk

Accretion in Binaries II

Correlation Time Scales of the X-ray Flux in Low Mass X-ray Binary

Evolution of X-ray Binaries and the Formation of Binary Pulsars

Neutron Star masses.

A possible model of pulsar timing

Final states of a star: 1. White Dwarf

Broad-band Spectroscopy of X-ray Binary Pulsars

Two types of glitches in a solid quark star model

Evolutionary Link between X-ray Pulsars and Millisecond Radio Pulsars

Presentation transcript:

On the formation of the peculiar LMXB IGR J17480-2446 in Terzan 5 ApJ772.6(2013) On the formation of the peculiar LMXB IGR J17480-2446 in Terzan 5 Reporter: Jiang Long(姜龙) Director: Prof. Li X-D 2019/4/11

Outline Recycled scenario J17480-2446 Patruno’s model Our explanation Binary-single scattering and J17480-like system formation Reversed-to-parallel evolution history Further discussion 2019/4/11

Recycled scenario of MSP After accretion a low magnetic high rotate MSP left.

Known Accreting MSP SAX J1808.4-3658 401Hz 2~3*108G BD IGR J00291+5934 599Hz 2*108G BD XTE J1751-305 435Hz 4*108G WD …

Cavecchi et~al. 2011;Patruno et~al. 2012 J17480-2446 Mass of companion 0.4-1.5 M⊙ Orbit period 21.3h Frequency derivation: 1.4*10-12HzS-1 Spin frequency: 11Hz 815Hz QPO ( B<5*108G) Located in the core of Terzan 5 Cavecchi et~al. 2011;Patruno et~al. 2012

Explanation of Patruno et al. 2012 Mildly recycled pulsar Magneto-dipole spin-down Wind accretion spin-down Current RLOF spin-up phase The magnetic dipole moment decayed in proportion to the rotation rate due to flux-line vortex line coupling (Srinivasan et al. 1990).

Shortcomings of Patruno’s model kHz QPO 815Hz GX 1+4 B~3*1013G, frequency: 6*10-3 Long-period X-ray pulsar: 4U2206+54, GX301-2, SXP1062 B>1014

Our explanation The current binary system is not the primordial one, the neutron star exchanged its donor during a binary-single close encounter. The neutron star had finished its spin-up evolution and become an MSP before the encounter. The orbit angular momentum of the later formed binary was reversed to the spin angular momentum of the neutron star

Heggie, Hut, McMillan, ApJ467,359(1996) Encounter rate v 1 2 3 Heggie, Hut, McMillan, ApJ467,359(1996)

Anti-parallel donor binaries

Evolution history Spin-up to MSP Spin-down with new donor Spin-up to current period

Further discussion (1) IGR J17480−2446-like systems Difference between two models Magnetic field Mass of companion

or Further discussion (2) Field decay: Shibazaki et al. (1989) Kiel et al. (2008) or

Thank you!