BVRI observations of PSR B0656+14 with the 6-meter telescope

V. G. Kurt, V. V. Sokolov, S. V. Zharikov, George Pavlov, B. V. Komberg

Research output: Contribution to journalArticle

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Abstract

We observed the middle-aged radio pulsar B0656+14 with a CCD detector at the 6-m telescope. Broadband BVRI images show the following magnitudes of the pulsar counterpart: B = 24.85(+0.19,-0.16), V = 24.90(+0.16,-0.14), R = 24.52(+0.12,-0.11), I = 23.81(+0.27,-0.21). We fitted the UV-optical (space + ground-based) data with a two-component model which combines a power law (non-thermal component) with a thermal spectrum emitted by the neutron star surface. The power law component, with the energy power-law index α = 1.5(+1.1,-1-2), dominates in the observed range. Constraints on the thermal component correspond to the RayleighJeans parameter G = T6(R10/d500)2 = 4.1(+2.1,-4.1), where T = 106T6 K is the brightness temperature, R∞ = 10R10 km is the neutron star radius as seen by a distant observer, and d = 500d500 pc is the distance. The shape of the optical-UV spectrum of PSR B0656+14 differs considerably from those observed from other pulsars: the middle-aged Geminga and young Crab, Vela.

Original languageEnglish (US)
Pages (from-to)547-556
Number of pages10
JournalAstronomy and Astrophysics
Volume333
Issue number2
StatePublished - Dec 1 1998

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power law
telescopes
pulsars
neutron stars
brightness temperature
crabs
crab
radio
charge coupled devices
broadband
radii
energy
detectors
parameter
young
detector
index

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Kurt, V. G., Sokolov, V. V., Zharikov, S. V., Pavlov, G., & Komberg, B. V. (1998). BVRI observations of PSR B0656+14 with the 6-meter telescope. Astronomy and Astrophysics, 333(2), 547-556.
Kurt, V. G. ; Sokolov, V. V. ; Zharikov, S. V. ; Pavlov, George ; Komberg, B. V. / BVRI observations of PSR B0656+14 with the 6-meter telescope. In: Astronomy and Astrophysics. 1998 ; Vol. 333, No. 2. pp. 547-556.
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Kurt, VG, Sokolov, VV, Zharikov, SV, Pavlov, G & Komberg, BV 1998, 'BVRI observations of PSR B0656+14 with the 6-meter telescope', Astronomy and Astrophysics, vol. 333, no. 2, pp. 547-556.

BVRI observations of PSR B0656+14 with the 6-meter telescope. / Kurt, V. G.; Sokolov, V. V.; Zharikov, S. V.; Pavlov, George; Komberg, B. V.

In: Astronomy and Astrophysics, Vol. 333, No. 2, 01.12.1998, p. 547-556.

Research output: Contribution to journalArticle

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N2 - We observed the middle-aged radio pulsar B0656+14 with a CCD detector at the 6-m telescope. Broadband BVRI images show the following magnitudes of the pulsar counterpart: B = 24.85(+0.19,-0.16), V = 24.90(+0.16,-0.14), R = 24.52(+0.12,-0.11), I = 23.81(+0.27,-0.21). We fitted the UV-optical (space + ground-based) data with a two-component model which combines a power law (non-thermal component) with a thermal spectrum emitted by the neutron star surface. The power law component, with the energy power-law index α = 1.5(+1.1,-1-2), dominates in the observed range. Constraints on the thermal component correspond to the RayleighJeans parameter G = T6(R10/d500)2 = 4.1(+2.1,-4.1), where T = 106T6 K is the brightness temperature, R∞ = 10R10 km is the neutron star radius as seen by a distant observer, and d = 500d500 pc is the distance. The shape of the optical-UV spectrum of PSR B0656+14 differs considerably from those observed from other pulsars: the middle-aged Geminga and young Crab, Vela.

AB - We observed the middle-aged radio pulsar B0656+14 with a CCD detector at the 6-m telescope. Broadband BVRI images show the following magnitudes of the pulsar counterpart: B = 24.85(+0.19,-0.16), V = 24.90(+0.16,-0.14), R = 24.52(+0.12,-0.11), I = 23.81(+0.27,-0.21). We fitted the UV-optical (space + ground-based) data with a two-component model which combines a power law (non-thermal component) with a thermal spectrum emitted by the neutron star surface. The power law component, with the energy power-law index α = 1.5(+1.1,-1-2), dominates in the observed range. Constraints on the thermal component correspond to the RayleighJeans parameter G = T6(R10/d500)2 = 4.1(+2.1,-4.1), where T = 106T6 K is the brightness temperature, R∞ = 10R10 km is the neutron star radius as seen by a distant observer, and d = 500d500 pc is the distance. The shape of the optical-UV spectrum of PSR B0656+14 differs considerably from those observed from other pulsars: the middle-aged Geminga and young Crab, Vela.

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Kurt VG, Sokolov VV, Zharikov SV, Pavlov G, Komberg BV. BVRI observations of PSR B0656+14 with the 6-meter telescope. Astronomy and Astrophysics. 1998 Dec 1;333(2):547-556.