Standard

Neutron stars: history of the magnetic field decay. / Igoshev, A.P.; Kholtygin, A.F.

в: Proceedings of the International Astronomical Union, Том 291, 2013, стр. 408-410.

Результаты исследований: Научные публикации в периодических изданиях › статья › Рецензирование

Harvard

Igoshev, AP & Kholtygin, AF 2013, 'Neutron stars: history of the magnetic field decay', Proceedings of the International Astronomical Union, Том. 291, стр. 408-410. https://doi.org/10.1017/S1743921312024301

APA

Igoshev, A. P., & Kholtygin, A. F. (2013). Neutron stars: history of the magnetic field decay. Proceedings of the International Astronomical Union, 291, 408-410. https://doi.org/10.1017/S1743921312024301

Vancouver

Igoshev AP, Kholtygin AF. Neutron stars: history of the magnetic field decay. Proceedings of the International Astronomical Union. 2013;291:408-410. https://doi.org/10.1017/S1743921312024301

Author

Igoshev, A.P. ; Kholtygin, A.F. / Neutron stars: history of the magnetic field decay. в: Proceedings of the International Astronomical Union. 2013 ; Том 291. стр. 408-410.

BibTeX

@article{43d4da3da38242b0a9abccf3ffa7b745,
title = "Neutron stars: history of the magnetic field decay",
abstract = "Using the data of the ATNF pulsar catalog we study the relation connected the real age t of young neutron stars (NS) and their spin-down age τ. We suppose that this relation is independent from both initial period of the NS and its initial surface magnetic field, and that the laws of the surface magnetic field decay are similar for all NSs in the Milky Way. We further assume that the birth-rate of pulsars was constant during at least last 200 million years. With these assumptions we were able to restore the history of the magnetic field decay for the galactic NSs. We reconstruct the universal function f(t) = B(t)/B 0, where B 0 is the initial magnetic field and B(t) is the magnetic field of NS at the age t. The function f(t) can be fitted by a power law with power index α = -1.17.",
keywords = "methods: data analysis, methods: statistical, stars: neutron, magnetic fields, pulsars: general",
author = "A.P. Igoshev and A.F. Kholtygin",
year = "2013",
doi = "10.1017/S1743921312024301",
language = "English",
volume = "291",
pages = "408--410",
journal = "Proceedings of the International Astronomical Union",
issn = "1743-9213",
publisher = "Cambridge University Press",

}

RIS

TY - JOUR

T1 - Neutron stars: history of the magnetic field decay

AU - Igoshev, A.P.

AU - Kholtygin, A.F.

PY - 2013

Y1 - 2013

N2 - Using the data of the ATNF pulsar catalog we study the relation connected the real age t of young neutron stars (NS) and their spin-down age τ. We suppose that this relation is independent from both initial period of the NS and its initial surface magnetic field, and that the laws of the surface magnetic field decay are similar for all NSs in the Milky Way. We further assume that the birth-rate of pulsars was constant during at least last 200 million years. With these assumptions we were able to restore the history of the magnetic field decay for the galactic NSs. We reconstruct the universal function f(t) = B(t)/B 0, where B 0 is the initial magnetic field and B(t) is the magnetic field of NS at the age t. The function f(t) can be fitted by a power law with power index α = -1.17.

AB - Using the data of the ATNF pulsar catalog we study the relation connected the real age t of young neutron stars (NS) and their spin-down age τ. We suppose that this relation is independent from both initial period of the NS and its initial surface magnetic field, and that the laws of the surface magnetic field decay are similar for all NSs in the Milky Way. We further assume that the birth-rate of pulsars was constant during at least last 200 million years. With these assumptions we were able to restore the history of the magnetic field decay for the galactic NSs. We reconstruct the universal function f(t) = B(t)/B 0, where B 0 is the initial magnetic field and B(t) is the magnetic field of NS at the age t. The function f(t) can be fitted by a power law with power index α = -1.17.

KW - methods: data analysis

KW - methods: statistical

KW - stars: neutron

KW - magnetic fields

KW - pulsars: general

U2 - 10.1017/S1743921312024301

DO - 10.1017/S1743921312024301

M3 - Article

VL - 291

SP - 408

EP - 410

JO - Proceedings of the International Astronomical Union

JF - Proceedings of the International Astronomical Union

SN - 1743-9213

ER -

ID: 5637547