Nucleon Superfluidity vs Thermal States of INSs & SXTs in quiescence

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1 Nucleon Superfluidity vs Thermal States of INSs & SXTs in quiescence K.P.Levenfish, D.G.Yakovlev, P.Haensel I Ioffe Institute, S.Petersburg Copernicus Astronomical Center, Warsaw

2 Brown, Bildstein, Rutledge`98 Spectrum of quiescent emission from SXTs is well fitted by a NS atmosphere model and may be thus of thermal origin, being supported by deep crustal heating due to nuclear transformations in the accreted crust. Yakovlev, Levenfish, Haensel `03 Direct correspondence of the problem of transienty accreting NSs to the problem of cooling isolated NSs. Quiescent SXTs test essentially the same physics as the ISNs: composition and superfluidity of superdense matter, crustal structure, composition and conductivity, light-elements accreted envelope etc. Ushomirsky & Rutledge`01, Colpi, Geppert, Page, Possenti `01, Brown, Bildsten, Chang `02, Rutledge etal `02, Yakovlev, Levenfish, Potekhin etal `04 Thermal states of transiently accreting NSs in SXTs vs observations of their quiescent thermal emission.

3 Deep crustal heating in transiently accreting NSs in SXTs Q dh = MeV/nucl Haensel, Zdunik 1990, 2003

4 Two subsets of NSs Cooling INSs Transiently accreting NSs in SXTs dt Thermal balance: Thermal balance: CT Lν T Lγ Ts dt dh dt CT ( ) = - Lν( T)- Lγ ( Ts ) Heating (cooling) to steady-state: L = (, ) dt γ Lγ t M Cooling: Ts = Ts () t In steady-state: ( ) = - ( )- ( ) + L ( M ) L ( M ) Lν( T) + Lγ ( Ts ) dh = L = L ( M ) γ γ Heating Curves Cooling Curves Cooling Curves

5 Standard scenario (cooling dominated by Modified Urca in a nonsuperfluid NS core) cannot explain thermal states of neither the INSs nor the SXTs in quiescence

6 Mere admittance for enhanced mechanisms of neutrino emission in nonsuperfluid NS doesnot help to explain observations Latimer, Prakash, Pethick, Haensel 1991 : direct Urca processes Page & Applegate 1992 : fast cooling scenario

7 Scenario with enhanced cooling of nosuperfluid star cannot explain observations neither of the ISNs nor accreting NSs in SXTs Steady-state of accreting NSs in SXTs

8 Composition of NSs cores: Nucleons? Hyperons? Cooling of INSs Steady-state of SXTs Yakovlev etal 2004

9 Srtong proton superfluidity : suppresses the modified Urca : slows down the cooling of the low-mass NSs smoothes the switching of the direct Urca : allows for existence of the representative class of the medium-mass NSs

10 Strong proton superfluidity : : T cp 9 10 K explains hot sources smoothes the opening of the enhanced cooling explains representative class of medium-mass NSs Thermal states of cooling INSs Steady-states of accreting NSs in SXTs Kaminker, Yakovlev, Gnedin 2002 Levenfish Yakovlev,Haensel 2006

11 Mild neutron superfuidity: appears at the neutrino stage of NSs thermal evolution ; reduces the NSs heat capacity almost in 4 times; boosts the neutrino emission due to the Cooper Pairing process. The neutron Cooper pairing process strongly accelerate the cooling of the low-mass NSs at the neutrino stage. Reduction of the heat capacity strongly accelerates the cooling at the photon stage

12 Mild neutron superfluidity : cn = ( 8 9) T K Contradicts observations of hot sources Should be absent in low-mass NSs (in the outer NS cores) Can lead to dichotomy of thermal states of SXTs Thermal states of cooling ISNs Steady-states of accreting NSs in SXTs YYakovlev etal 2002 Levenfish,Yakovlev Haensel 2006

13 Mild neutron superfluidity in the inner NSs cores

14 Minimal cooling scenario (enhanced cooling due to neutron Cooper pairing): Marginally compatible with the data on INSs Contradicts the data on SXTs in quiescence The enhanced cooling should be more powerful than the neutron Cooper pairing Thermal states of cooling INSs Steady-state of SXTs Gusakov etal 2004; Page etal 2004 Levenfish, Yakovlev, Haensel 2006

15 SUMMARY The data on INSs and SXTs test essentially the same physics of the internal structure of NSs and can be analyzed together These data can probe: the EOS and composition of a NS core, superfluidity of baryons, the level of neutrino emission, the models of accreted crust Both INSs and SXTs require the presense of strong proton superfluidity Both INSs and SXTs rule out the models of mild neutron superfluidity in the cores of low-mass NSs The data on SXTs seem to rule out Cooper-pairing neutrino emission as an enhanced cooling agent

16 Dichotomy of thermal evolution of accreting NSs: Effect of the mild neutron superfluidity (mild Cooper pairing) Steady-states of a SXT vs mass accretion rate M BARRED THERMAL STATES Levenfish, Yakovlev, Haensel 2006

17 Dichotomy of thermal evolution of accreting NSs: Effect of the mild neutron superfluidity (mild Cooper pairing) Steady-states of SXTs vs initial core temperature T BARRED THERMAL STATES Levenfish, Yakovlev, Haensel 2006

18 Good questions : Observations: Average mass accretion rates Narrow observational constaints on themal emission in quiescence Nonthermal components of quiescent emission Variable thermal emission in quiescence Theory: Deep crustal heating models Cooper pairing in the NSs crust

19 Everywhere in neutron star cores. Most important in low-mass stars. Modified Urca process n + N p + e + N p + e + N n + N + ν + ν e e erg Q ~ 10 T9 3 cm s L ν 38 ~ T 8 9 erg s Bremsstrahlung N + N N + N +ν +ν erg Q ~ 10 T9 3 cm s L ν 36 ~ T 8 9 erg s ν e, ν µ, ν τ Inner cores of massive neutron stars: Nucleons, hyperons Pion condensates Kaon condensates n p + e + ν p + e n + ν n~ ~ p + e + ν e ~ p + e n~ + ν q~ q~ + e + ν e q~ + e q~ + ν e e e e 27 6 erg Q ~ 3 10 T9 3 cm s erg Q ~ 10 T9 3 cm s erg Q ~ 10 T9 3 cm s L L L ν ν ν ~ 10 ~ 10 ~ T T T erg s erg s erg s Quark matter d u + e + ν u + e d + ν e e erg Q ~ 10 T9 3 cm s L ν ~ T 6 9 erg s

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21 Gusakov, Kaminker, Yakovlev, Gnedin 2005