1 / 14

A young pulsar with a long radio trail emerging from SNR G315.9-0.0

A young pulsar with a long radio trail emerging from SNR G315.9-0.0. F. Camilo, C.-Y. NG et al. arxiv :0908.2421v1. Introduction. Discussion. Observations and results. 01. 02. 03. 目录. Introduction. Frying pan SNR G315.9-0.0 contour 2.5 5 7.5 10 15 and 20mJy

derora
Download Presentation

A young pulsar with a long radio trail emerging from SNR G315.9-0.0

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. A young pulsar with a long radio trail emerging from SNR G315.9-0.0 F. Camilo, C.-Y. NG et al.arxiv :0908.2421v1

  2. Introduction Discussion Observations and results 01 02 03 目录

  3. Introduction • Frying pan SNR G315.9-0.0 • contour 2.5 5 7.510 15 and 20mJy • Shell ~13'Jet like tail ~8' no IRcounterpart Mills 1981 MOST@843MHz

  4. MOST @843MHzWhiteoak&Green 1996

  5. Observations and results Image fromATCA 2.4 GHz ATNF Parkes2008 June 17 6.1 hr @1374MHzwith 288MHz BW

  6. Identified pulsar PSR J1437-5959 • P~61msDM=549pc cm-3D~8kpc(from Cordes&Lazio NE2001 electron density model)~50% linearly polarized throughout the pulse profile

  7. 9.6ks Swift observation on 2008 July 5 • only one photon within 5" of the pulsar position • NH =1.6 × 1022 cm−2photon index Γ＝1.5assume 5 photons as the limitfX < 4.5 × 10−14 erg cm−2 s−1 LX < 3.5 × 1032 d8^2 erg s−1 LX / Edot < 2.5 × 10−4 d8^2

  8. Discussion • Suggesting PSR association with the SNR • NE2001 model uncertainty for the system~25%d8 = 1 ± 0.25 • τc = 114 kyrτ114 = τ/τc • Vt = 300 d8/τ114 km s−1 • RSNR = 17 d8 pc • the SNR shell radius is small for such the age 114 kyr

  9. Sedov solution constraints on age • τ≈ 22 d85/2(n0/E51)1/2 kyrhydrogen ambient medium densityn0cm-3SN explosion kinetic energy 1051E51

  10. Other constraints on age • the trail ~RSNR = 17 d8 pc • τc = 114 kyrThe pulsar wind trail collimated for about 50kyr. Detailed study of PWN will find if it's resonable.(under way using ATCA) • If τ114 = τ/τc<<1, e.g. τ114∽0.2, Vt≈ 1500 km s−1The proper motion is µ = 8/τ114 mas yr−1 ,this could be measurable with the ATCA.

  11. PSR J1437–5959 has a very small flux density • luminosityL1.4 ≡ S1.4d2≈5d8^2 mJy kpc2now unremarkable following numerous young pulsar discoveries in recent years • Parkes multibeam survey 1997(Manchester et al. 2001)

  12. the faint tail of the populationremains out of reach in a significant Galactic volume

  13. 谢谢观赏

More Related