Kuehnel: Created page with "Category:Accreting X-ray Pulsars Other Names: V* X Per [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=X+Per&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Simbad..."

2018-04-18T11:57:27Z

Created page with "Category:Accreting X-ray Pulsars Other Names: V* X Per [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=X+Per&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Simbad..."

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[[Category:Accreting X-ray Pulsars]]

Other Names: V* X Per [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=X+Per&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Simbad], 4U 0352+309

'''Monitoring data''':
[http://xte.mit.edu/asmlc/srcs/xper.html RXTE/ASM]
[http://swift.gsfc.nasa.gov/docs/swift/results/transients/XPer/ Swift/BAT]
[http://maxi.riken.jp/top/index.php?cid=1&jname=J0355+310 MAXI]

= Coordinates =
RA 03h 55' 23.077", DEC +31° 02' 45.01" 
RA 58.8461542deg, DEC -31.0458361deg 
l 163.0814, b -17.1362 

= Binary system =

Distance: 0.95(20) kpc (<ref name="Telting98" />)

== Orbit ==

{| class="wikitable"
! Parameter
! Value
! Unit
! Reference
|-
| Porb
| 250
| days
| <ref name="DelgadoMarti2001" />
|-
| tau
|
| MJD
|
|-
| a sin i
| 2
| AU
| <ref name="DelgadoMarti2001" />
|-
| e
| 0.11
|
| <ref name="DelgadoMarti2001" />
|-
| omega
|
| deg
|
|}

= Description =

4U 0352+309 is a persistent X-ray source in a binary with the Be-type star X Persei. It is believed that the neutron strar accretes material from the wind of either the Be companion atmosphere (fast, low-density) or its outskirts, i.e. the Be-disk (low, dense). A good summary and discussion about the different scenarios can be found in <ref name="Doroshenko2012" />. 

== Spectrum ==

The spectrum of 4U 0352+309 is unusually hard and is detectable up to 200 keV in ISGRI. Earlier models describe the spectrum by a combination of two powerlaws (<ref name="DiSalvo98" />) or a black body with an additional hard powerlaw (<ref name="Coburn01" />). The later also requires an absorption like feature around 30 keV, which was interpreted as CRSF. A recent analysis by <ref name="Doroshenko2012" /> showed, however, that the unusual spectrum can be described well by two thermal Comptonization models. Thereby the claimed cyclotron line is no longer needed. In addition, the used model, the relatively long pulse period of 837 s and by comparing to [[4U 2206+54]] may suggest the neutron star to have a magnetic field in the order of 1014 G, thus in the '''magnetar''' range.

'''References'''

X Per - Revision history

Kuehnel: Created page with "Category:Accreting X-ray Pulsars Other Names: V* X Per [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=X+Per&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Simbad..."