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A Stellar Wind Bubble Coincident with the Anomalous X-Ray Pulsar IE 1048.I-5937: Are Magnetars Formed from Massive Progenitors?

Citation

Gaensler, BM and McClure-Griffiths, NM and Oey, MS and Haverkorn, M and Dickey, JM and Green, AJ, A Stellar Wind Bubble Coincident with the Anomalous X-Ray Pulsar IE 1048.I-5937: Are Magnetars Formed from Massive Progenitors?, The Astrophysical Journal, 620, (2) pp. L95-L98. ISSN 0004-637X (2005) [Refereed Article]

DOI: doi:10.1086/428725

Abstract

We present 21 cm H I observations from the Southern Galactic Plane Survey of the field around the anomalous X-ray pulsar 1E 1048.1 -5937, a source whose X-ray properties imply that it is a highly magnetized neutron star (a "magnetar"). These data reveal an expanding hydrogen shell, GSH 288.3-0.5-28, centered on 1E 1048.1-5937, with a diameter of 35 × 23 pc (for a distance of 2.7 kpc) and an expansion velocity of ≈7.5 km s -1. We interpret GSH 288.3-0.5-28 as a wind bubble blown by a 30-40 M ⊙; star, but no such central star can be readily identified. We suggest that GSH 288.3-0.5-28 is the wind bubble blown by the massive progenitor of 1E 1048.1-5937 and consequently propose that magnetars originate from more massive progenitors than do radio pulsars. This may be evidence that the initial spin period of a neutron star is correlated with the mass of its progenitor and implies that the magnetar birthrate is only a small fraction of that for radio pulsars. © 2005, The American Astronomical Society. All rights reserved.

Item Details

Item Type:Refereed Article
Research Division:Physical Sciences
Research Group:Astronomical and Space Sciences
Research Field:Galactic Astronomy
Objective Division:Expanding Knowledge
Objective Group:Expanding Knowledge
Objective Field:Expanding Knowledge in the Physical Sciences
Author:Dickey, JM (Professor John Dickey)
ID Code:35905
Year Published:2005
Web of Science® Times Cited:101
Deposited By:Physics
Deposited On:2005-08-01
Last Modified:2006-03-29
Downloads:0

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