NDLI: Are the magnetic fields of millisecond pulsars ∼108 G?

Content Provider	Springer Nature Link
Author	Souza, Rafael S. Opher, Reuven
Copyright Year	2010
Abstract	It is generally assumed that the magnetic fields of millisecond pulsars (MSPs) are ∼108 G. We argue that this may not be true and the fields may be appreciably greater. We present six evidences for this: (1) The ∼108G field estimate is based on magnetic dipole emission losses which is shown to be questionable; (2) The MSPs in low mass X-ray binaries (LMXBs) are claimed to have <1011 G on the basis of a Rayleygh-Taylor instability accretion argument. We show that the accretion argument is questionable and the upper limit 1011 G may be much higher; (3) Low magnetic field neutron stars have difficulty being produced in LMXBs; (4) MSPs may still be accreting indicating a much higher magnetic field; (5) The data that predict ∼108 G for MSPs also predict ages on the order of, and greater than, ten billion years, which is much greater than normal pulsars. If the predicted ages are wrong, most likely the predicted ∼108 G fields of MSPs are wrong; (6) When magnetic fields are measured directly with cyclotron lines in X-ray binaries, fields ≫108 G are indicated. Other scenarios should be investigated. One such scenario is the following. Over 85% of MSPs are confirmed members of a binary. It is possible that all MSPs are in large separation binaries having magnetic fields >108 G with their magnetic dipole emission being balanced by low level accretion from their companions.
Starting Page	267
Ending Page	271
Page Count	5
File Format	PDF
ISSN	0004640X
Journal	Astrophysics and Space Science
Volume Number	330
Issue Number	2
e-ISSN	1572946X
Language	English
Publisher	Springer Netherlands
Publisher Date	2010-07-22
Publisher Place	Dordrecht
Access Restriction	One Nation One Subscription (ONOS)
Subject Keyword	Magnetic fields Millisecond pulsars Astronomy, Observations and Techniques
Content Type	Text
Resource Type	Article
Subject	Astronomy and Astrophysics Space and Planetary Science

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