Standard

Population Synthesis of Neutron Stars: the Impact of Different Luminosity Models. / Igoshev, A.P.; Kholtygin, A.F.

Proceedings of a Conference held at University of Zielona Góra, Zielona Góra, Poland, 24-27 April 2012. San Francisco: Astronomical Society of the Pacific, 2012.. Astronomical Society of the Pacific, 2012. стр. 147-148.

Результаты исследований: Публикации в книгах, отчётах, сборниках, трудах конференций › статья в сборнике › научная

Harvard

Igoshev, AP & Kholtygin, AF 2012, Population Synthesis of Neutron Stars: the Impact of Different Luminosity Models. в Proceedings of a Conference held at University of Zielona Góra, Zielona Góra, Poland, 24-27 April 2012. San Francisco: Astronomical Society of the Pacific, 2012.. Astronomical Society of the Pacific, стр. 147-148. <http://adsabs.harvard.edu/abs/2012ASPC..466..147I>

APA

Igoshev, A. P., & Kholtygin, A. F. (2012). Population Synthesis of Neutron Stars: the Impact of Different Luminosity Models. в Proceedings of a Conference held at University of Zielona Góra, Zielona Góra, Poland, 24-27 April 2012. San Francisco: Astronomical Society of the Pacific, 2012. (стр. 147-148). Astronomical Society of the Pacific. http://adsabs.harvard.edu/abs/2012ASPC..466..147I

Vancouver

Igoshev AP, Kholtygin AF. Population Synthesis of Neutron Stars: the Impact of Different Luminosity Models. в Proceedings of a Conference held at University of Zielona Góra, Zielona Góra, Poland, 24-27 April 2012. San Francisco: Astronomical Society of the Pacific, 2012.. Astronomical Society of the Pacific. 2012. стр. 147-148

Author

Igoshev, A.P. ; Kholtygin, A.F. / Population Synthesis of Neutron Stars: the Impact of Different Luminosity Models. Proceedings of a Conference held at University of Zielona Góra, Zielona Góra, Poland, 24-27 April 2012. San Francisco: Astronomical Society of the Pacific, 2012.. Astronomical Society of the Pacific, 2012. стр. 147-148

BibTeX

@inbook{d17d70d1a1f64f5aba0cf6d11bfea97d,
title = "Population Synthesis of Neutron Stars: the Impact of Different Luminosity Models",
abstract = "We study the birth and evolution of isolated neutron stars in the Milky Way with new population synthesis code. We model the birth of massive OB stars and follow their motion within the spiral arms up to the supernova explosion. After that we consider the evolution of NS up to the death line with taking into account the magnetic field decay. We find that significant magnetic field decay occurs during the first stages of a NS's life. Derived values of mean time of ohmic decay for NS is two hundred thousand years. To simulate the ensemble of the galactic pulsars we consider the different scenarios of the pulsar's radio luminosity. First of them is a standard flat cone model by Narayan & Ostriker (1990) with exponential energy distribution in the cone and the second is a spark model by Fan et al. (2001). To select the best of them we compare the distributions of pulsar periods (P), derivatives of periods (ṗ) and pulsar magnetic fields (B) with obtained from ATNF pulsar catalogue data. We conclude that the realis",
keywords = "neutron stars: population synthesis",
author = "A.P. Igoshev and A.F. Kholtygin",
year = "2012",
language = "English",
pages = "147--148",
booktitle = "Proceedings of a Conference held at University of Zielona G{\'o}ra, Zielona G{\'o}ra, Poland, 24-27 April 2012. San Francisco: Astronomical Society of the Pacific, 2012.",
publisher = "Astronomical Society of the Pacific",
address = "United States",

}

RIS

TY - CHAP

T1 - Population Synthesis of Neutron Stars: the Impact of Different Luminosity Models

AU - Igoshev, A.P.

AU - Kholtygin, A.F.

PY - 2012

Y1 - 2012

N2 - We study the birth and evolution of isolated neutron stars in the Milky Way with new population synthesis code. We model the birth of massive OB stars and follow their motion within the spiral arms up to the supernova explosion. After that we consider the evolution of NS up to the death line with taking into account the magnetic field decay. We find that significant magnetic field decay occurs during the first stages of a NS's life. Derived values of mean time of ohmic decay for NS is two hundred thousand years. To simulate the ensemble of the galactic pulsars we consider the different scenarios of the pulsar's radio luminosity. First of them is a standard flat cone model by Narayan & Ostriker (1990) with exponential energy distribution in the cone and the second is a spark model by Fan et al. (2001). To select the best of them we compare the distributions of pulsar periods (P), derivatives of periods (ṗ) and pulsar magnetic fields (B) with obtained from ATNF pulsar catalogue data. We conclude that the realis

AB - We study the birth and evolution of isolated neutron stars in the Milky Way with new population synthesis code. We model the birth of massive OB stars and follow their motion within the spiral arms up to the supernova explosion. After that we consider the evolution of NS up to the death line with taking into account the magnetic field decay. We find that significant magnetic field decay occurs during the first stages of a NS's life. Derived values of mean time of ohmic decay for NS is two hundred thousand years. To simulate the ensemble of the galactic pulsars we consider the different scenarios of the pulsar's radio luminosity. First of them is a standard flat cone model by Narayan & Ostriker (1990) with exponential energy distribution in the cone and the second is a spark model by Fan et al. (2001). To select the best of them we compare the distributions of pulsar periods (P), derivatives of periods (ṗ) and pulsar magnetic fields (B) with obtained from ATNF pulsar catalogue data. We conclude that the realis

KW - neutron stars: population synthesis

M3 - Article in an anthology

SP - 147

EP - 148

BT - Proceedings of a Conference held at University of Zielona Góra, Zielona Góra, Poland, 24-27 April 2012. San Francisco: Astronomical Society of the Pacific, 2012.

PB - Astronomical Society of the Pacific

ER -

ID: 4623456