dc.contributor.author |
Sivaram, C |
|
dc.contributor.author |
Kochhar, R. K |
|
dc.date.accessioned |
2008-10-25T13:05:24Z |
|
dc.date.available |
2008-10-25T13:05:24Z |
|
dc.date.issued |
1984-01 |
|
dc.identifier.citation |
Astrophysics and Space Science, Vol. 98, No. 1, pp. 203 - 205 |
en |
dc.identifier.issn |
0004-640X |
|
dc.identifier.uri |
http://hdl.handle.net/2248/3977 |
|
dc.description.abstract |
There are indications that less than 10/sup-3 of the spin-down energy of the millisecond pulsar PSR 1937+214 emerges as electromagnetic radiation. The implications of this result are discussed. The surface magnetic field would then be ≡10/sup7G, making the pulsar optically undetectable, and casting aspersions on the accretion disc spin-up neutron star models for the pulsar. The pulsar should have an equatorial ellipticity ɛ ≡ 10/sup-9, which can be accounted for if the equatorial magnetic field departs from axisymmetry by one part in 10/sup3. |
en |
dc.language.iso |
en |
en |
dc.publisher |
Springer |
en |
dc.relation.uri |
http://www.springerlink.com/content/q65410213g355462/ |
en |
dc.subject |
Astrophysics |
en |
dc.subject |
Pulsars |
en |
dc.subject |
Stellar Magnetic Fields |
en |
dc.subject |
Accretion Disks |
en |
dc.subject |
Electromagnetic Radiation |
en |
dc.subject |
Energy Dissipation |
en |
dc.subject |
Stellar Models |
en |
dc.subject |
Stellar Rotation |
en |
dc.title |
On the slow-down of the millisecond pulsar PSR 1937 + 214 |
en |
dc.type |
Article |
en |