Neutron Stars—Cooling and Transport

Potekhin, A. Y.; Pons, José A.; Page, Dany

doi:10.1007/s11214-015-0180-9

Cited by 275 publications

(358 citation statements)

References 212 publications

Supporting

Mentioning

349

Contrasting

Order By: Relevance

“…Meanwhile, thermal emission for intermediate age (∼ 10 5 yr) neutron stars gives L X ∼ 10 31 − 10 33 erg s −1 (see, e.g. Potekhin et al 2015). The more recent observations since late 2015 show significant brightening in X-rays (see Fig.…”

Section: Discussionmentioning

confidence: 96%

Multiwavelength monitoring and X-ray brightening of Be X-ray binary PSR J2032+4127/MT91 213 on its approach to periastron

Lyne

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

The radio and gamma-ray pulsar PSR J2032+4127 was recently found to be in a decadeslong orbit with the Be star MT91 213, with the pulsar moving rapidly towards periastron. This binary shares many similar characteristics with the previously unique binary system PSR B1259−63/LS 2883. Here, we describe radio, X-ray, and optical monitoring of PSR J2032+4127/MT91 213. Our extended orbital phase coverage in radio, supplemented with Fermi LAT gamma-ray data, allows us to update and refine the orbital period to 45-50 yr and time of periastron passage to 2017 November. We analyse archival and recent Chandra and Swift observations and show that PSR J2032+4127/MT91 213 is now brighter in X-rays by a factor of ∼ 70 since 2002 and ∼ 20 since 2010. While the pulsar is still far from periastron, this increase in X-rays is possibly due to collisions between pulsar and Be star winds. Optical observations of the Hα emission line of the Be star suggest that the size of its circumstellar disc may be varying by ∼ 2 over timescales as short as 1-2 months. Multiwavelength monitoring of PSR J2032+4127/MT91 213 will continue through periastron passage, and the system should present an interesting test case and comparison to PSR B1259−63/LS 2883.

show abstract

Section: Discussionmentioning

confidence: 96%

Multiwavelength monitoring and X-ray brightening of Be X-ray binary PSR J2032+4127/MT91 213 on its approach to periastron

Lyne

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

show abstract

“…Isolated neutron stars with 10 − 100 yr < ∼ t < ∼ 10 5 yr have isothermal interiors and cool mainly from inside via neutrino emission (e.g., Refs. [3][4][5]). To study their cooling, one needs L ∞ ν ( T ) and C core ( T ).…”

Section: Introductionmentioning

confidence: 99%

Neutrino luminosities and heat capacities of neutron stars in analytic form

et al. 2017

View full text Add to dashboard Cite

We derive analytic approximations for the neutrino luminosities and the heat capacities of neutron stars with isothernal nucleon cores as functions of the mass and radius of stars. The neutrino luminosities are approximated for the three basic neutrino emission mechanisms, and the heat capacities for the five basic combinations of the partial heat capacities. The approximations are valid for for a wide class of equations of state of dense nucleonmatter. The results significantly simplify the theoretical interpretation of observations of cooling neutron stars as well as of quasistationary thermal states of neutron stars in X-ray transients. For illustration, we present an analysis of the neutrino cooling functions of nine isolated neutron stars taking into account the effects of their magnetic fields and of the presence of light elements in their heat blanketing envelopes. These results allow one to investigate the superfluid properties of neutron star cores.

show abstract

“…Superfluid transitions reconstruct low energy structures of neutrons and considerably affects evolution and cooling of neutron stars. Superfluidity indeed gives a key to understand long relaxation time observed in the sudden speed-up events of neutron stars [23][24][25], and enhancement of neutrino emmission at the onset of superfluid transition might explain the the recently observed cooling process [26][27][28][29]. The existence of superfluid components may also explain sudden changes of spin periods observed in pulsars [30,31].…”

mentioning

confidence: 99%

P23superfluids are topological

2017

View full text Add to dashboard Cite

We clarify topology of 3 P2 superfluids which are expected to be realized in the inner cores of neutron stars and cubic odd-parity superconductors.3 P2 phases include uniaxial/biaxial nematic phases and nonunitary ferromagnetic and cyclic phases. We here show that all the phases are accompanied by different types of topologically protected gapless fermions: Surface Majorana fermions in nematic phases and a quartet of (single) itinerant Majorana fermions in the cyclic (ferromagnetic) phase. Using the superfluid Fermi liquid theory, we also demonstrate that dihedral-two and -four biaxial nematic phases are thermodynamically favored in the weak coupling limit under a magnetic field. It is shown that the tricritical point exists on the phase boundary between these two phases and may be realized in the core of realistic magnetars. We unveil the intertwining of symmetry and topology behind mass acquisition of surface Majorana fermions in nematic phases.

show abstract

Neutron Stars—Cooling and Transport

Cited by 275 publications

References 212 publications

Multiwavelength monitoring and X-ray brightening of Be X-ray binary PSR J2032+4127/MT91 213 on its approach to periastron

Multiwavelength monitoring and X-ray brightening of Be X-ray binary PSR J2032+4127/MT91 213 on its approach to periastron

Neutrino luminosities and heat capacities of neutron stars in analytic form

P23superfluids are topological

Contact Info

Product

Resources

About