Pulsar research at soft -rays Lucien Kuiper, Wim Hermsen Hans Bloemen


НазваPulsar research at soft -rays Lucien Kuiper, Wim Hermsen Hans Bloemen
Дата конвертації06.06.2013
Розмір468 b.
ТипПрезентации


Pulsar research at soft -rays

  • Lucien Kuiper, Wim Hermsen Hans Bloemen


Outline of presentation

  • Introduction: pulsars in a nutshell

  • Overview current high-energy status (> 10 keV)

  • Concluding remarks



Pulsars (rapidly spinning neutron stars with high B-fields)

  • Pulsars (rapidly spinning neutron stars with high B-fields)

  • can be grouped into three sub-classes:

  • I: spin-down powered pulsars a) normal pulsars b) millisecond pulsars (old recycled systems)

  • II: accretion powered pulsars a) LMXB (incl. transient ms-pulsars) b) HMXB (Be-binaries; (sub-)giant binaries) III: magnetically powered pulsars (=magnetars) AXPs/SGRs



Spin-down powered (energetic) pulsars (Class Ia)

  • CGRO (1991-2000; 20 keV-30 GeV) heritage: number of -ray pulsars increased from 2 (Crab;Vela) to 7 (10) : all associated with young (≤ 100 ky) and energetic pulsars; exception ms-pulsar PSR J0218+4232

  • The only established galactic source population emitting -rays over a wide (0.5 keV – 10 GeV) energy band

  • Inspite ~30 year research we still do NOT know where the -rays are produced in the magnetosphere (outer gap/polar cap) and which physical processes are acting (synchrotron, curvature, inverse Compton, photon splitting etc.)







To understand the HE emission characteristics (pulse profile morphology changes vs. energy phase resolved spectroscopy; double/triple peaked or asymmetric single peaked profiles) requires a significant increase of the number of -ray pulsars

  • To understand the HE emission characteristics (pulse profile morphology changes vs. energy phase resolved spectroscopy; double/triple peaked or asymmetric single peaked profiles) requires a significant increase of the number of -ray pulsars

  • Recent post-CGRO progress (Chandra/XMM/RXTE/INTEGRAL): Targetted (very) deep searches at the cores of SN-remnants or error boxes of unid. EGRET sources yielded the detection of several radio dim/quiet energetic pulsars emitting hard X-rays (> 10 keV): e.g.







Spin-down powered millisecond pulsars (Class Ib)





  • Anomalous X-ray pulsars (status before early 2004) - No rotation powered pulsar! LX >> Lsd - No X-ray pulsar in LMXB/HMXB steady spin-down; no apparent (no accretion-powered pulsar) optical counterpart; no periodic Doppler delay in X-ray timing

  • Characteristics:

    • Pulse periods: 5 -12 s
    • “Steady” spin-down like rotation powered pulsars (glitches observed also)
    • X-ray luminosities: 1034-36 erg/s (steady, but outbursts also detected; transient AXPs)
    • (very) soft X-ray (0.5-10 keV) spectra: BB (0.35 – 0.6 keV) + PL (2 – 4)
    • Similar to Soft Gamma-Ray Repeaters Magnetars (neutron stars (glitches; (out)bursts) with B ~ 1014-15 Gauss powered by decay of B-field)
    • Young population concentrated along galactic plane; some embedded in Supernova remnants






High-energy spectra Kes 73 and AXP 1E 1841-045 (Kuiper, Hermsen & Mendez, 2004, ApJ 613, 1173)







1E2259+586 (CTB 109) RXTE PCA/HEXTE



1E2259+586 (CTB 109)



Conclusion



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