The mass and radius of neutron star in 4U

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The mass and radius of neutron star in 4U 1746-37 Quark and Compact Stars 2014 The mass and radius of neutron star in 4U 1746-37 Zhaosheng Li (李兆升) Department of Astronomy Peking University 2014-10-20

Outlines Why? How to constrain M-R of NS in LMXB? The M-R of NS in 4U 1746-37

Equation of States Self-bound or Gravity bound

Mass Main sequence NS binaries WD-NS binaries DNS binaries Black widow pulsar X-ray/Optical binaries Anna Watts et al.2014

How to constrain the M-R of NS? Redshift measurement Pulse Profile in X-ray pulsars Atmosphere emission in qLMXBs PRE bursts

LMXB transient source “Switched on”: Accretion outburst “Switched off”: Quiescence

Gravitational Redshift EXO 0748-676 (XMM-Newton) Z=0.35 Fe XXVI (Hα) 9.518, 9.533, 9.579 9.675, 9.690, 9.73813.0 Fe XXV (He-like) O VIII Cottam et al. (2002)

Only once in EXO 0748-676 Cottam et al. (2008) None detection of absorption line !

Pulse Profile in X-ray Pulsars NICER, Gendreau et al. (2012)

Fan Beam + Pencil Beam + . Leahy 2004

qLMXBs in Globular Clusters Deep Crustal Heating Brown et al. (1998) nsatmos Guillot et al. (2013)

qLMXBs in Globular Clusters nsatmos Guillot et al. (2013) Lattimar & Steiner (2013)

qLMXBs in Globular Clusters nsatmos Guillot et al. (2013) H/He atmosphere Lattimar & Steiner (2013)

Summary Redshift M/R Pulse Profile in X-ray pulsars M/R Atmosphere emission in qLMXBs M-R PRE bursts

Type I vs. Type II X-ray burst Type I (nuclear burning) Type II (accretion event) MXB 1730-335 Rapid Burster Sala et al.2012

PRE X-ray Burst Photospheric Radius Expansion Expansion->Contraction->Cooling The radiation pressure is larger than the gravitational one. Photospheric layers are lifted off the surface by the radiation pressure. 4U 1728-34 Guver et al. 2012

Mass-Radius confidence intervals Bayes(Ozel et al.(2009,2010)) or Monte-Carlo simulation

RXTE Obs. Of 4U 1746-37/NGC6441 Dipping binary Low touchdown flux (luminosity) Low mass NS?

Results 4U 1746-37/NGC 6441

Obscuration 4U 1746-37/NGC 6441

Conclusions An extremely low mass NS may exist in 4U 1746-37 EoSs can be effectively tested from low mass NS Formation Lower limit mass (self-bound or gravity bound NS) Radius