A similar scenario has also been put forward by Shternin et al. In particular, a critical temperature T c = 5 × 10 8 K for the triplet neutron superfluidity is implied in this process. 2004) and explained that the onset of enhanced neutrino emission resulting from the neutron pairing in the core is enough to explain the cooling data. (2011) interpreted the Cas A data within the frame of the minimal cooling paradigm ( Page et al.
![cassiopeia stars cassiopeia stars](https://i.pinimg.com/originals/80/f5/98/80f598ec8cc3200f9608f86af547276c.jpg)
It is also unlikely that the observed cooling can be attributed to fast cooling models alone, such as direct Urca (DU) processes or neutrino emission from Bose condensates, for instance. 2006 Yakovlev & Pethick 2004) or to the medium modified Urca model ( Grigorian & Voskresensky 2005). This cooling rate is significantly stronger than expected when compared to the standard cooling model ( Page et al. In particular, the authors argued that the surface temperature has rapidly decreased from 2.12 × 10 6 to 2.04 × 10 6 in almost one decade, from 2000 to 2009. The estimated values of radius and mass vary from R = 8.3 km and M = 2.01 M ⊙ to R = 10.3 km and M = 1.65 M ⊙ depending on the reduction procedure of Chandra X-ray Observatory archival data ( Heinke & Ho 2010). 2006) and its thermal X-ray spectrum is consistent with a nonmagnetized carbon atmosphere with a surface temperature of 2 × 10 6 K ( Ho & Heinke 2009). Its estimated age of 330 yrs is in agreement with its kinematic age ( Fesen et al. The neutron star identified with the historical supernova SN 1680 in Cassiopea A (Cas A) is the youngest one to be discovered in the Milky Way.
![cassiopeia stars cassiopeia stars](http://www.caelumobservatory.com/obs/cassAmatthews.jpg)
Key words: dense matter / equation of state / stars: neutron / stars: magnetic field / supernovae: individual: Cassiopeia A We thus argue that it is difficult to put severe constraints on the superfluid gap if the Joule heating is considered. It is shown that it is possible to explain a fast cooling regime as the one observed in the neutron star in Cassiopea A if the Joule heating produced by dissipation of the small-scale magnetic field in the crust is taken into account. In particular, we consider neutron star models obtained from the equation of state computed in the framework of the Brueckner-Bethe-Goldstone many-body theory and variational methods, and models obtained with the Akmal-Pandharipande-Ravenhall equation of state. The thermomagnetic evolution of the young neutron star in Cassiopea A is studied by considering fast neutrino emission processes. Ioffe Institute of Physics and Technology, 194021 St. Urpin 1 ,3ġ INAF, Osservatorio Astrofisico di Catania, via S.Sofia 78, 95123 Catania, ItalyĮ-mail: INFN, Sezione di Catania, via S.Sofia 72, 95123 Catania, Italyģ A. Astronomical objects: linking to databasesĪ.
![cassiopeia stars cassiopeia stars](https://images.immediate.co.uk/production/volatile/sites/25/2021/07/Cassiopeia-chart-ecc06a8.jpg)
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