Formation of Redback and Black Widow Binary Millisecond Pulsars

Slides:

Advertisements

Similar presentations

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

Advertisements

ASTR Fall Semester Joel E. Tohline, Alumni Professor Office: 247 Nicholson Hall [Slides from Lecture17]

J.E. Horvath, IAG – USP São Paulo, Brazil with O. Benvenuto & M.A. De Vito (La Plata) Measurements and theory of neutron stars masses.

Weighing in on Neutron Stars Varun Bhalerao California Institute of Technology Collaborators: F. Harrison, S. Kulkarni, Marten van Kerkwijk, and others.

Small is Beautiful: Cataclysmic Variables from the SDSS John Southworth Boris Gänsicke Tom Marsh + many others.

RXTE Observations of Cataclysmic Variables and Symbiotic Stars Koji Mukai NASA/GSFC/CRESST and UMBC.

Christian Knigge University of Southampton School of Physics & Astronoy P. Marenfeld and NOAO/AURA/NSF Christian Knigge University of Southampton Low-Mass.

Discovery of a Highly Eccentric Binary Millisecond Pulsar in a Gamma-Ray- Detected Globular Cluster Megan DeCesar (UWM) In collaboration with Scott Ransom.

Christian Knigge University of Southampton School of Physics & Astronoy Disk Stability vs Close Binary Evolution Rob Hynes (LSU) Christian Knigge University.

Millisecond pulsar population and related high energy phenomena 王伟 (NAOC) July 2009, Pulsar Summer School Beijing.

Accretion Processes in GRBs Andrew King Theoretical Astrophysics Group, University of Leicester, UK Venice 2006.

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.

Mass transfer in a binary system

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.

Pulsars Basic Properties. Supernova Explosion => Neutron Stars part of angular momentum carried away by shell field lines frozen into solar plasma (surface.

Neutron Stars and Black Holes

LECTURE 20, NOVEMBER 9, 2010 ASTR 101, SECTION 3 INSTRUCTOR, JACK BRANDT 1ASTR 101-3, FALL 2010.

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

Neutron Stars 2: Phenomenology Andreas Reisenegger Depto. de Astronomía y Astrofísica Pontificia Universidad Católica de Chile Chandra x-ray images of.

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.

Understanding LMXBs in Elliptical Galaxies Vicky Kalogera.

The Deaths of Stars Chapter 10. Mass Transfer in Binary Stars In a binary system, each star controls a finite region of space, bounded by the Roche Lobes.

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.

1 The faintest accretors A.R. King & R. Wijnands astro-ph/

Neutron Stars 2: Phenomenology Andreas Reisenegger ESO Visiting Scientist Associate Professor, Pontificia Universidad Católica de Chile Chandra x-ray.

25 Facts about Parkes, Pulsars and

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

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.

Transitional Millisecond pulsars as accretion probes

Star Clusters and their stars Open clusters and globular clusters General characteristics of globular clusters Globular cluster stars in the H-R diagram.

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

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.

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.

Binary millisecond X-ray pulsars Department of Physics University College Cork Paul Callanan and Mark Reynolds Alexei Filippenko, Department of Astronomy,

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

Sub-Eddington accretion flows in neutron-star low-mass X-ray binaries Rudy Wijnands Astronomical Institute “Anton Pannekoek” University of Amsterdam 25.

J.E. Horvath, IAG – USP São Paulo, Brazil with O. Benvenuto & M.A. De Vito (La Plata) Why "black widow" pulsar systems are important for the quest of neutron.

ON THE LOW LEVEL X-RAY EMISSION OF TRANSITIONAL PULSARS Enrico Bozzo University of Geneva.

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

On Young Neutron Stars as Propellers and Accretors Ma Bo, Department of Astronomy, Nju, Nanjing Citations: Alpar,M.A.,APJ554,1245,2000 Illarionov and Sunyaev.1975.

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.

Probing the neutron star physics with accreting neutron stars (part 1) Alessandro Patruno University of Amsterdam The Netherlands.

Orbital evolution of compact Black-hole binaries and white dwarf binaries Wencong Chen Astro-ph/ Astro-ph/

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

Black Holes Accretion Disks X-Ray/Gamma-Ray Binaries.

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

Evolutionary Sequences For Low- And-Intermediate-Mass X-Ray Binaries Ph. Podsiadlowski S. Rappaport E. D. Pfahl.

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

Hyperaccreting Disks around Neutrons Stars and Magnetars for GRBs: Neutrino Annihilation and Strong Magnetic Fields Dong Zhang (Ohio State) Zi-Gao Dai.

Stellar Corpses and Other Space Oddities

References: 1. Bhattacharya & van den Heuvel, Phys Reports, vol 203, 1, X-ray Binaries, edited by Lewin, van Paradijs, and van den Heuvel, 1995,

Welcome! 1962: 1 st LMXB (Accretion power) 1968: 1 st PSR (Rotation power) 1972: Accretion disc theory 1978: Cyclotron lines, ~Thermonuclear Bursts 1982:

HOW TO DETECT A BLACK HOLE Effects on matter/light outside the horizon –gravitational attraction of other bodies –“dark star” with mass distinguish from.

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.

Basic Properties By Dr. Lohse, University of Berlin

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

A possible model of pulsar timing

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

Evolutionary Link between X-ray Pulsars and Millisecond Radio Pulsars

Presentation transcript:

Formation of Redback and Black Widow Binary Millisecond Pulsars Kun Jia and Xiang-Dong Li Department of Astronomy Nanjing University 2015-9-25 KIAA-WAP

Millisecond Pulsar (MSP)-Low-mass X-ray Binary (LMXB) Relation Recycling Scenario (Alpar 1982; Radakrishnan & Srinivasan 1982) – Spin up to ms periods – Magnetic field decay High mass star PSR LMXB MSP 2015-9-25 KIAA-WAP 2

Observational evidence for the recycling scenario Millisecond X-ray pulsations from LMXBs SAX J1808.4-3658 Wijnands & van der Klis 1998 Patruno & Watts 2012 2013-04-25 2015-9-25 KIAA-WAP KIAA 3 3

Observational evidence for the recycling scenario Transitions between rotation and accretion power in MSPs PSR J1023+ 0038 (Archibald et al. 2009) IGR J18245-2452/PSR J1824–2452I (Papitto et al. 2013) XSS J12270-4859 (Bogdanov et al. 2014) 2015-9-25 X-ray radio KIAA-WAP

The three transitional pulsars are also eclipsing MSPs Roberts 2013 Redbacks non-degenerate companion (~0.2 M⊙-0.4 M⊙) Black widows (semi)-degenerate companion (~0.02 M⊙-0.05 M⊙) 2015-9-25 KIAA-WAP

The eclipsing material possibly originates from the companions evaporated by the high-energy particles from the MSPs 2015-9-25 KIAA-WAP

Gamma-ray MSPs > ⅓ of known MSPs are Gamma-ray MSPs For Ė>5×1033 erg/s is >¾ (!) Most Fermi MSPs are black widows and redbacks 2015-9-25 KIAA-WAP

A significant variation in the accretion rate is required to explain the transitional behavior in LMXBs. Linares 2014 2015-9-25 KIAA-WAP

The disrupted magnetic braking (MB) model (Chen et al. 2013) MB GR 2015-9-25 KIAA-WAP

The irradiation-induced cyclic mass transfer model (Benvenuto et al 2015-9-25 KIAA-WAP

The accretion-induced collapse (AIC) model (Smedley et al. 2015) Collapse of an accreting white dwarf (WD) to form a MSP The companion star becomes detached from its Roche lobe because of sudden orbital expansion Formation rates uncertain Difficult or impossible for the occurrence of AIC in traditional CVs 2015-9-25 KIAA-WAP

Transient LMXBs Outburst Quiescence 2015-9-25 KIAA-WAP

The parameter space for the disk instability Covers the distribution of known redbacks If the MSP activity switches on during the quiescent phase of LMXBs, they may evolve to be redbacks 2015-9-25 KIAA-WAP

Evolution with evaporation Evaporative wind mass loss rate v2,esc - escape velocity at the surface of the companion star Lp - NS’s spin-down luminosity f - efficiency of evaporation 2015-9-25 KIAA-WAP

Cases with f = 0.1 2015-9-25 KIAA-WAP

Changing f and angular momettum 2015-9-25 KIAA-WAP

Results Binary evolution sensitively depends on the angular momentum of the evaporative wind and f The redback companions The redback orbital periods Redback - black widow relation 2015-9-25 KIAA-WAP

Conclusions Almost all LMXBs are subject to the thermal and viscous instability during their evolution The resultant redbacks can possess main-sequence, evolved, and (proto-)WD companions with either Roche lobe filling or under-filling Part of redbacks may become black widows, while others form MSP/He WD binaries 2015-9-25 KIAA-WAP