Table 8: Comparison of the optical and X-ray spectral indices ( $ {\rm\alpha ^{O}_{\nu }}$, ${\rm\alpha ^{X}_{\nu }}$), luminosities ( ${L^{\rm O}}$, $ {L^{\rm X}} $), efficiencies ( ${ \rm\eta ^{O} } $, ${ \rm\eta ^{X} } $), and a weighted ratio ( $ {L^{\rm O}\Delta E^{\rm X}/L^{\rm X}\Delta E^{\rm O}} $) of the two young pulsars, Crab and PSR B0540-69.3, and the older Vela pulsar. Here $\Delta E^{\rm O}$ and $\Delta E^{\rm X}$ are the energy intervals in the opticala and X-raysb, respectively, used for the frequency integration to obtain ${L^{\rm O}}$ and $ {L^{\rm X}} $. Information on the period P, dynamical age $ {\rm\tau } $, spindown luminosity $\dot E$, and distance d for each pulsar is included.
PSR P $ {\rm\tau } $ $\dot E$ d $ {\rm\alpha ^{O}_{\nu }}$ ${L^{\rm O,a}}$ ${ \rm\eta ^{O} } $ ${\alpha^{\rm X}_{\nu}}$ ${L^{\rm X,b}}$ ${ \rm\eta ^{X} } $ ${L^{\rm O}\Delta E^{\rm X} \over L^{\rm X}\Delta E^{\rm O}}$
  ms kyr ${\rm 10^{37}~erg~s^{-1}}$ kpc   ${\rm 10^{33}~erg~s^{-1}} $ ${\rm 10^{-5} } $   ${\rm 10^{36}~erg~s^{-1}} $ ${\rm 10^{-3} } $  
Crab 33.49 1.24 46 2 -0.21c 7.9c 1.7 0.87d 1.0d 2.17 34.9
0540 50.2 1.66 15 51 1.07e 10.9e 7.3 0.83d 3.13d 21 15.5
Vela 89 11 0.69 0.29 0.25f ${\rm 7.0^f\times 10^{-5}}$ ${\rm 1.0\times 10^{-3}}$ 0.5g ${\rm 2.3^g\times 10^{-5}}$ ${\rm 3.4 \times10^{-3}}$ 13.5

a For the optical range 1.57-3.68 eV. e This paper.
b For the X-ray range 0.6-10 keV. f Using data from Shibanov et al. (2003).
c Using data from Sollerman (2003) for 1.57-3.68 eV. g Pavlov et al. (2001a); $ {L^{\rm X}} $ rescaled to the 0.6-10 keV range
d Kaaret et al. (2001); $ {L^{\rm X}} $ rescaled to the 0.6-10 keV range. and d=0.29 kpc.


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