| Issue |
A&A
Volume 407, Number 1, August III 2003
|
|
|---|---|---|
| Page(s) | 259 - 263 | |
| Section | Stellar structure and evolution | |
| DOI | https://doi.org/10.1051/0004-6361:20030829 | |
| Published online | 17 November 2003 | |
What we can learn from observations of cooling neutron stars
1
Ioffe Physical Technical Institute, Politekhnicheskaya 26, 194021 St.-Petersburg, Russia
2
Copernicus Astronomical Center, Bartycka 18, 00-716 Warsaw, Poland e-mail: haensel@camk.edu.pl
Corresponding author: D. G. Yakovlev, yak@astro.ioffe.ru
Received:
3
September
2002
Accepted:
17
April
2003
A generic toy model of a cooling neutron star (NS) is used to analyze cooling of NSs with nucleon and exotic compositions of the cores. The model contains the parameters which specify the levels of slow and fast neutrino emission as well as the lower and upper densities of the layer where the slow emission transforms into the fast one. The prospects to constrain these parameters from the present and future observations of isolated middle-aged NSs are discussed.
Key words: stars: neutron / dense matter
© ESO, 2003
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.