CaltechAUTHORS
  A Caltech Library Service

Staring at 4U 1909+07 with Suzaku

Fürst, F. and Pottschmidt, K. and Kreykenbohm, I. and Müller, S. and Kühnel, M. and Wilms, J. and Rothschild, R. E. (2012) Staring at 4U 1909+07 with Suzaku. Astronomy and Astrophysics, 547 . Art. No. A2. ISSN 0004-6361. https://resolver.caltech.edu/CaltechAUTHORS:20130116-141359975

[img]
Preview
PDF - Published Version
See Usage Policy.

309kB

Use this Persistent URL to link to this item: https://resolver.caltech.edu/CaltechAUTHORS:20130116-141359975

Abstract

We present an analysis of the neutron star high mass X-ray binary (HMXB) 4U 1909+07 mainly based on Suzaku data. We extend the pulse period evolution, which behaves in a random-walk like manner, indicative of direct wind accretion. Studying the spectral properties of 4U 1909+07 between 0.5 to 90 keV we find that a power-law with an exponential cutoff can describe the data well, when additionally allowing for a blackbody or a partially covering absorber at low energies. We find no evidence for a cyclotron resonant scattering feature (CRSF), a feature seen in many other neutron star HMXBs sources. By performing pulse phase resolved spectroscopy we investigate the origin of the strong energy dependence of the pulse profile, which evolves from a broad two-peak profile at low energies to a profile with a single, narrow peak at energies above 20 keV. Our data show that it is very likely that a higher folding energy in the high energy peak is responsible for this behavior. This in turn leads to the assumption that we observe the two magnetic poles and their respective accretion columns at different phases, and that these accretion columns have slightly different physical conditions.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1051/0004-6361/201219845DOIArticle
ORCID:
AuthorORCID
Fürst, F.0000-0003-0388-0560
Pottschmidt, K.0000-0002-4656-6881
Kreykenbohm, I.0000-0001-7335-1803
Wilms, J.0000-0003-2065-5410
Additional Information:© 2012 ESO. Received 20 June 2012. Accepted 16 September 2012. Published online 18 October 2012. This work was supported by the Bundesministerium für Wirtschaft und Technologie through DLR grants 50OR0808, 50OR0905, and 50OR1113. F.F. thanks GSFC for the hospitality. This research has made use of data obtained from the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). This work is furthermore based on observations with INTEGRAL, an ESA project with instruments and science data centre funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland, Spain), Czech Republic and Poland, and with the participation of Russia and the USA. We have made use of NASA’s Astrophysics Data System. We like to thank J. E. Davis for the slxfig module which was used to create all plots throughout this paper.
Group:Space Radiation Laboratory
Funders:
Funding AgencyGrant Number
Bundesministerium für Wirtschaft und Technologie (BMWi)50OR0808
Bundesministerium für Wirtschaft und Technologie (BMWi)50OR0905
Bundesministerium für Wirtschaft und Technologie (BMWi)50OR1113
ESA Member StatesUNSPECIFIED
Deutsches Zentrum für Luft- und Raumfahrt (DLR)UNSPECIFIED
Subject Keywords:accretion, accretion disks X-rays: binaries stars: neutron
Record Number:CaltechAUTHORS:20130116-141359975
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20130116-141359975
Official Citation:Staring at 4U 1909+07 with Suzaku F. Fürst, K. Pottschmidt, I. Kreykenbohm, S. Müller, M. Kühnel, J. Wilms and R. E. Rothschild Published online: 18 October 2012 DOI: http://dx.doi.org/10.1051/0004-6361/201219845
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:36432
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:16 Jan 2013 22:35
Last Modified:28 Jan 2021 23:02

Repository Staff Only: item control page