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Neutrino Cooling of Neutron Stars PowerPoint Presentation
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Neutrino Cooling of Neutron Stars

Neutrino Cooling of Neutron Stars

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Neutrino Cooling of Neutron Stars

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  1. Neutrino Cooling of Neutron Stars D.N. Voskresensky NRNU MEPhI, Moscow

  2. General information on NS “Standard” scenario. “Minimal” cooling. Neutrino reaction rates in normal nuclear matter in superfluid nuclear matter “Nuclear medium cooling” scenario. Medium effects on reaction rates in normal nuclear matter in superfluid nuclear matter conclusions Plan

  3. Neutron stars are forming in supernova II explosions (M~Msol, R~10 km, initialT~30-50 MeV) «Простираю свою персону ниц: я наблюдал в созвездии Твен-Куан явление звезды-гостьи.» Янг-Вэй-Тэ Pulsar in Crab cancellationis remnantSN 1052 observed in 1968

  4. Double neutron star binaries 1,4414(2) M☉,1,3867(2) M☉ majority of measured NS masses are focused near the value 1.4 Msol

  5. New data: masses are essentially different Pulsar J1614-2230 Measured Shapiro delay with high precision P.Demorest et al., Nature 467 (2010) Time signal is getting delayed when passing near massive object. Pulsar J0348-04232 M = (2.01± 0.04 ) Msol J. Antoniadis et al., Science (2013) Highest well-known masses of NS there are heavier, but far less precisely measured candidates) Lowest well-known mass of NS 1.18 ±0.02 Мsol

  6. NS mass-central density diagram for different EoS Klähn et al. PRC 74, 035802 (2006) If M>2.4 Msol ( ) were observed, all these EoS would be invalid! Central densities in various NS are different! Studying various NS we may test density dependences of EoS and NN interaction

  7. HEAVY ION COLLISIONS MEET NEUTRON STARS (common constraints) Danielewicz, Lacey, Lynch (2002) - Boltzmann kinetic equation fitted to directed & elliptic flow Stiffest EoS do not satisfy the HIC constraint. Only EoS near the upper boundary of the box satisfy both the HIC and NS mass constraints yielding Mmax>1.93 Msol

  8. Aim: to construct a phenomenological EoS and apply it to calculations of neutron stars and hydro. calculations of HIC reactions a RMF-based (KVOR, Mmax~2 Msol ) quasiparticle model with scaled hadron masses and couplings Kolomeitsev,D.V.Nucl.Phys. (2005); T.Klahn, et al. Phys.Rev. (2006) following constraints from chiral symmetry restoration, SU(3) multiplet particle species are included Khvorostukhin,Toneev,D.V. Nucl. Phys. (2007,2008)

  9. 1) age of the associated SNR 3) historical events Crab : 1054 AD Cassiopeia A: 1680 AD Tycho’s SN: 1572 AD 2) pulsar speed and position w.r. to the geometric center of the associated SNR rotation frequency period for non-accreting systems, period increases with time power-law spin-down braking index for magnetic dipole spin-down n=3 “spin-down age"

  10. Yakovlev et al

  11. Explosion ofSN1987A Registration of 20 neutrinosEν~ 10-40 МэВ If Supernova will be exploded in our Galaxy (frequency 1/(30-100 yr)), Superkamiokandewill register ~103 neutrinos! certainly, if not too close to our Sun  !!!

  12. Cooling of neutron stars After passing a minute, during 105 years a neutron star cools down by neutrino emission, than by photon emission from the surface (except first minutes after NS formation during which NS cools down up to few MeV) White-body radiation problem (at low T<T ~1-few MeV): direct reactions: Similar to di-lepton radiation problem in HIC opac bring information straight from the dense interior Tsurf (t) is related to Tin (t); problem to compute Tin (t)

  13. emissivity For T> min., T<Topac~ MeV neutron star is transparent for neutrino cV - specific heat density, εv – neutrino emissivity, Ф, λ – metric coefficients for t>300-500yr CV – specific heat, L-luminosity ~60 MeV each fermion leg on a Fermi surface ~ T neutrino phase space ´ neutrino energy

  14. slow cooling Neutron star cooling data 3 groups+Cas A: >103 in emissivity CaS A intermediate cooling rapid cooling How to describe all groups within one cooling scenario?

  15. (where baryon density Cooling: crust is light and interior is massive most important are reactions in dense interior n0 is the nuclear saturation density) G.Gamov Phase-space separation direct Urca (DU) one-nucleon reactions: modified Urca (MU) two-nucleon reactions: nucleon bremsstrahlung (NB) (less important) • URCA “Un-Recordable Coolant Agent” (by Gamov) Casino da Urca in Brazil-waist of money; pilferer, thief in Odessa

  16. the weak interaction constant lepton current nucleon current ~v (Fermi velocity) corrections are important Note 1/2 in neutral channel, since Z boson is neutral and W is charged!

  17. For bare vertices ! emissivity: Counting powers ofT: each external nucleon and electron line ~T neutrino phase space ´ neutrino energy • one-nucleon phase-space volume (» 1027-1028 factor) • T6dependence • threshold behavior (n>ncDU , ncDU depends on EoS) • very moderate density dependence

  18. D.V., Senatorov Yad.Fiz.(1987) self-energy with free non-equilibrium Green’s functions Cut of the diagram means removing of dE integration due to -function

  19. Pion Urca processes PU is also one-nucleon process (if the model permits pion condensation) For pion Urca (PU) processes: All “exotic” one-nucleon processes start only when the density exceeds some critical density

  20. energy-momentum conservation requires processes on neutral currents are forbidden!

  21. Friman & Maxwell AJ (1979) FOPE model of NN interaction (no medium effects) (1) (3) k (2) (4) Additionally one should take into account exchange reactions (identical nucleons) FOPE model continues to be used by different groups, e.g. by Page et. All, Yakovlev et al.

  22. Emissivity: s=2 is symmetry factor. Reactions with the electron in an initial state yield extra factor 2. Finally due to exchange reactions Coherence:only axial-vector term contributes (!)

  23. + - + - + - + - + - + + - - + - - + + - + - + - + - - + - + + - + - + - thick pion line (here up to 2nd order): one-nucleon process with pion two-nucleon process

  24. Nucleon-nucleon pairing in NS(for T<Tc ~109-1010 K) A.B. Migdal 1959

  25. Pairing in NS matter A.B.Migdal (1959) model I model II 3P2 gap is <10 keV

  26. Standard scenario + exotics standard MU: exotics DU: PU:

  27. DU constraint: DU process schould be „exotics“(if DU starts it is dificult to stop it) since in reality masses of NS are not close to each other EoS should produce a large DU threshold in NS matter ! MDU>1.35-1.5 Msol Otherwise why many masses have M~1.3-1.5 Msol ? [Kolomeitsev, D.V. (2005), Klahn et al. (2006)]

  28. DU -- information about nuclear EoS should be modified Information about density dependence of the symmetry energy 3 n0 Klähn et al. PRC 74, 035802 (2006) L>80 MeV are excluded by the DU constraint

  29. - + normal matter with free vertices and Green’s functions are forbidden new “quasi”-one-nucleon-like processes (one-nucleon phase space volume) become permitted superfluid matter [Flowers, Ruderman, Sutherland, AJ 205 (1976), D.V.& Senatorov, Sov. J. Nucl. Phys. 45 (1987) ] Diagrams with normal and anomalous Green func. - - + + Naive generalization: are allowed

  30. In superfluid (T<Tc<0.1-1 MeV) all two-nucleon processes are suppressed by factor exp(-2/T) un-paired nucleon paired nucleon D.V., Senatorov (1987) nn is neutron gap and nn=exp(-nn/T)

  31. strongly depending on Δ(n) pair breaking and formation (PBF) processes are important for cooling! D.V.& Senatorov, (1987) Schaab et al. (1996) [Page, Geppert, Weber , NPA 777, 497 (2006)]

  32. Minimal cooling paradigmD.Page et al., D.G. Yakovlev et al. Reactions in presence of pairing MU: PBF: (at least) and for Δ> 0.1 MeV attempts to fit cooling data by fitting Δ (n) dependencies and using different Ts-Tin for different NS • Minimal cooling paradigm does not allow to explain all available data • (problems or with slow coolers or with Cas A, + with rapid coolers).

  33. Minimal (+exotics) scenario for T<Tc standard minimal MU: PBF: (at least) exotics DU: PU:

  34. Minimal cooling +exoticsD.Page et al., D.G. Yakovlev et al. • Minimal cooling +exotics cannot appropriately explain all available modern data(either precision Cas A data or all others, with deficiency of the DU mentioned above).

  35. The only diagram in FOPE model which contributes to the MU and NB is Free one-pion exchange For consistency one needs to calculate corrections of the second-order in f NN in other values. Otherwise -- problems with unitarity. Pion polarization operator in dispersion relation at order f NN2 : measure of pion softening Pion condensation already at n>0.3 n0 But there is no pion condensation in atomic nuclei

  36. One should replace FOPE by the full NN interaction, essential part of which is due to MOPE with vertices corrected by NN correlations. NN-1 part of the pion polarization operator is Another inconsistency of standard scenario: it uses FOPE but adds PU processes for n > ncPU> n0: Pion condensation arises only due to pion softening!

  37. Dressed Green’s functions Dressed interactions Dressed vertices

  38. Direct reactions from piece of matter (v in NS, e+e-, γ, K+ in HIC) white body radiation problem General consideration: Knoll, D.V. Ann. Phys. 249 (1996) expansion in full non-equilibrium G - + Only for low T<<εF, quasiparticle approximation is valid (each G- + yields T2, allows to cut diagrams over G -+ ) For soft radiation: quasiclassics (all graphs in first line are of the same order):LPM effect

  39. Landau-Pomeranchuk-Migdal effect on example of the soft photon radiation ω~T>>Ѓ~T2/εF QPA region

  40. Part of the interaction involving  isobar is analogously constructed: pion with residual (irreducible in NN-1 and  N-1) s-wave  N interaction and  scattering`` Fermi liquid approach explicit nucleon-nucleon hole and Delta-nucleon hole degrees of freedom small

  41. full pion propagator: enhancement of the amplitude dressed vertex: suppression Low energy excitations in nuclear Fermi liquid (Landau-Migdal approach) based on a separation of long and short scales Re-summed NN interaction provided short-scale interaction can be reduced to the local one Similar to Debye screening in plasma Landau-Migdal parameters of short-range interaction are extracted from atomic nuclei Poles yield zero-sound modes in scalar and spin channels known phenomena in Fermi liquid see Migdal et al., Phys.Rep. (1990)

  42. similar for π0 in neutron matter free π Kolomeitsev,D.V. (1996) the smaller collision energy, the larger is in-medium effect 2 : ω <0 for n>n cr A.B. Migdal ZhETF (1971)

  43. Charged pion spectra in neutron matter and pion condensation [Migdal,Markin,Mishustin,JETP (1974)] variational calculations [Akmal, Pandharipande, Ravenhall, PRC58 (1998)]: pion condensate: neutral pion condensate:

  44. Pion softening with increase of the density reconstruction of pion spectrum on top of the pion condensate pion gap for n<ncPU no pion condensate |*|~ amplitude of the condensate 1st-order phase transition possibility of no π-cond. Г –vertex suppression factor From the cooling fit nc >2.5 n0

  45. MEDIUM EFFECTS IN NEUTRINO PRODUCTION In the medium many reaction channels are opened up

  46. The weak coupling vertex is renormalized in medium: wavy line corresponds to weak current For the -decay: For processes on the neutral currents with the correlation functions [D.V., Senatorov, Sov. J. Nucl. Phys. 45 (1987)]