Neutron Star Astronomy Roberto Mignani


НазваNeutron Star Astronomy Roberto Mignani
Дата конвертації06.06.2013
Розмір461 b.
ТипПрезентации


Neutron Star Astronomy

  • Roberto Mignani

  • University College London

  • Mullard Space Science Laboratory


The Role of HST in NS Astronomy



The Impact of HST on NS Astronomy

  • Higher sensitivity wrt pre 10-m class telescopes

  • Sharper spatial solution

  • UV + IR access

  • Timing

  • Polarimetry (poorly exploited)

  • All together, capabilities offered only by HST



Perspectives after SM-4

  • By the end of 2008, HST will be the longest-lived

  • astronomical satellite

    • WFPC2  WFC3 (UV+VIS+IR)
    • COSTAR  COS (UV)
    • STIS and ACS to be repaired
  • Spatial resolution: WFC3 (STIS+ACS)

  • UV: WFC3, COS (STIS+ACS)

  • IR: WFC3

  • WFC3 better in UV & IR wrt ACS & NICMOS

  • WFC3 worse in VIS wrt ACS, better wrt WFPC2

  • Timing: STIS

  • Polarimetry: ACS



Astrometry

  • HST proper motions (parallaxes) measured so far for 8 (4) neutron stars

  • WFC3 (ACS) can enlarge the sample with a much better accuracy

    • Confirm NS identifications
    • Localization of NS birth place
    • NS velocity  ISM accretion or not. Important for RX neutron stars
    • Hints on SN dynamics and progenitor core collapse


Neutron Stars Nebulae

  • WFC3 (ACS) can resolve the structure and variability of the Pulsar Wind Nebulae, as WFPC2 did for the Crab. Only chance for distant PWNe !

  • WFPC2 also found evidence of optical variability also in the B0540-69 PWN (De Luca et al. 2007;Mignani et al. 2008a)

  • Genuine variability in the nebula ?

  • Expanding optical jet from the pulsar (v=22000 km/s)?



The Near-UV



The Near-IR

  • NICMOS discovered IR emission from NSs

  • (Koptsevich et al. 2001), the first after the Crab

  • E.g., for B0656+14 the IR is a hint of

  • a debris disk of ≈2 10-4 Msun (Perna et al. 2000)

  • Disk not resolved by Spitzer (Mignani et al. 2008b)

  • Detection of debris disks has

  • implications on NS formation and

  • SN models

  • WFC3 can do a better job



Timing



Polarimetry

  • Optical polarimetry with ACS is a powerful diagnostic to:

  • test neutron star magnetosphere models

  • constrain magnetic field geometry

  • constrain the neutron star rotation angle wrt the sky

  • (iv) investigate pulsar/nebula magneto-dynamical interactions

  • Observations of PSR B0540-69 performed with WFPC2 (Mignani et al. 2008c)



More Goals …

  • While keeping the course on “classical” PSRs, there are other challenges to face

  • Many more classes of radio-quiet NSs are now known

  • Isolated Cooling NS (ICONSs): old NSs, no longer radio-active

  • Magnetars: transient HE sources, with B ≈ 1014 G

  • Compact Central Objects: Not Crab-like ! Nature is unclear

  • Rotating RAdioTransients (RRATs): bursting (otherwise quiescent) radio PSRs

  • High-B radio PSRs: magnetars by definition not by reputation

  •  UV-to-IR observations become more and more important !

  •  Critical to determine the NS nature (isolated, binary, isolated+disk)

  •  HST archaeo-astronomy to identify (via PM) NS parental clusters, study their properties, trace the origin of the NS diversity



Conclusions

  • HST has played so far a fundamental role in NS astronomy

  • After SM4, HST can play a role as (or even more) fundamental

    • The WFC3 (with ACS) will be unique for astrometry and stellar population studies
    • WFC3+COS will allow to obtain NSs multi-λ SED, especially in the crucial UV and IR bands
    • The repaired ACS+STIS will offer timing+polarimetry, crucial for NS astronomy and so far little explored due to technical failures
  • HST has posed the questions, now it can find the answers



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