HST and VLT observations of isolated neutron stars

R. P. Mignani, George Pavlov, A. De Luca, P. A. Caraveo

Research output: Contribution to journalArticle

1 Citation (Scopus)

Abstract

New results of optical observations of isolated pulsars and their environments are presented. Very Large Telescopes observations of PSR J0108-1431 set an upper limit of B ∼ 28.6 on its optical flux, implying a neutron star surface temperature T < 8.8 × 10 4 K (for d = 200 pc, R = 13 km). HST proper motion measurement of the PSR 1929+10 counterpart secured its optical identification. Finally, deep observations of the Vela pulsar field did not confirm the presence of an optical pulsar wind nebula (PWN).

Original languageEnglish (US)
Pages (from-to)518-522
Number of pages5
JournalAdvances in Space Research
Volume33
Issue number4
DOIs
StatePublished - Jan 1 2004

Fingerprint

pulsars
neutron stars
Stars
Neutrons
surface temperature
proper motion
nebulae
Telescopes
telescopes
Fluxes
Pulsars
Temperature

All Science Journal Classification (ASJC) codes

  • Aerospace Engineering
  • Astronomy and Astrophysics
  • Geophysics
  • Atmospheric Science
  • Space and Planetary Science
  • Earth and Planetary Sciences(all)

Cite this

Mignani, R. P. ; Pavlov, George ; De Luca, A. ; Caraveo, P. A. / HST and VLT observations of isolated neutron stars. In: Advances in Space Research. 2004 ; Vol. 33, No. 4. pp. 518-522.
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HST and VLT observations of isolated neutron stars. / Mignani, R. P.; Pavlov, George; De Luca, A.; Caraveo, P. A.

In: Advances in Space Research, Vol. 33, No. 4, 01.01.2004, p. 518-522.

Research output: Contribution to journalArticle

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AU - Mignani, R. P.

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AU - De Luca, A.

AU - Caraveo, P. A.

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AB - New results of optical observations of isolated pulsars and their environments are presented. Very Large Telescopes observations of PSR J0108-1431 set an upper limit of B ∼ 28.6 on its optical flux, implying a neutron star surface temperature T < 8.8 × 10 4 K (for d = 200 pc, R ∞ = 13 km). HST proper motion measurement of the PSR 1929+10 counterpart secured its optical identification. Finally, deep observations of the Vela pulsar field did not confirm the presence of an optical pulsar wind nebula (PWN).

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