The Zoo of neutron stars

Abstract

In these lecture notes I briefly discuss the present day situation and new discoveries in astrophysics of neutron stars focusing on isolated objects. The latter include soft gamma repeaters, anomalous X-ray pulsars, central compact objects in supernova remnants, the Magnificent seven, and rotating radio transients. In the last part of the paper I describe available tests of cooling curves of neutron stars and discuss different additional constraints which can help to confront theoretical calculations of cooling with observational data. 1

Theory of pulsar magnetosphere and wind

“…As the end product of stellar evolution, neutron stars form a special class of compact objects showing themselves with many different faces (Popov 2008;Harding 2013). The idea of the existence of neutron stars formed by the gravitational collapse of a star at the end of its life during the explosion of the supernova (Baade & Zwicky 1934) was suggested well before the observational evidence that appeared only thirty years later (Hewish et al 1968).…”

Isolated neutron stars in the galaxy: from magnetars to antimagnetars

“…It came out that young NSs can appear as sources of different nature (see a brief review in [1]). The reason for drastic differences between different types of young NSs is not yet understood.…”

Dipole photon strength functions from neutron induced reactions

“…Here we have to confess that theoretical study of E1 PSF has been initiated by experimental results [1,2] of Dubna group on investigation of the two step (n,γα)-reaction for target nucleus 143 Nd .The total width of this reaction could be expressed in form [2]: …”

“…Using the formula (45) for and calculating the transmission coefficients for α-emission by standard method [14] it could be obtained [2] PSF E1 shown below together with other experimental data for 144 Nd.…”

“…In many cases it is possible to study gamma-decay of individual excited (compound) induced reaction (n,γ) provides very detailed information on photon strength functions (PSF) with E γ nuclear states with known Jπ values leading to final states with very limited range of Jπ quantum numbers. In addition study of two-step (n, γα)-reaction [1,2] and (n, γγ)-decay [3][4][5][6] gives unique possibility to extract the information on PSF for γ-transitions between excited nuclear states important for verification of theoretical models and many practical applications. During last decade very useful the results on the sum of mainly dipole PSF were obtained with aid of two step reactions ( where and are quasi-particle-phonon basic functions, the principal and small components respectively.…”