Stars as Laboratories for Fundamental Physics - MPP Theory Group

56 Chapter 2
2.3.2 X-Ray Observations
Because the surface temperature of neutron stars is in the keV regime
they can be observed only by x-ray satellites such as the Einstein Observatory
which was launched in 1979, and more recently by EXOSAT and
Table 2.4. Selected x-ray observations of SN remnants and pulsars. a
Age [yr] Dist.
Remnant (in 1995) [kpc] Pulsar b Teff ∞ [10 6 K]
c d
3C58 (814) (2.6) — 2.2 ± 0.2 E 1
Crab 941 1.7–2 0531+21 < 1.6 R 2
(r, o, x, γ)
RCW 103 1500 ± 500 2 — 2.15 ± 0.15 E 1
< 1.2 R 3
MSH15–52 1850 ± 250 4.2 (r, x) detected E 1
Vela X ∼ 12,000 0.5 0833–45 0.95 ± 0.15 E 1
(r, o, x, γ) 1.6 ± 0.2 R 4
Monogem ∼ 110,000 (0.5) 0656+14 0.90 ± 0.04 R 5
Ring () (r, x) (0.30 ± 0.05)
— ∼ 340,000 0.15–0.4 Geminga 0.52 ± 0.10 R 6
(x, γ)
— ∼ 540,000 0.5–1.5 1055–52 0.65 ± 0.15 X 7
(r, x, γ) 0.75 ± 0.06 R 8
a Adapted from Tsuruta (1986) and updated.
b Pulsed radiation: r = radio, o = optical, x = x-rays, γ = γ-rays.
c E = Einstein, R = ROSAT, X = EXOSAT observation.
d References:
1. See the review by Tsuruta (1986) for references to the original literature.
2. Becker and Aschenbach (1995).
3. Becker et al. (1992).
4. Ögelman, Finley, and Zimmermann (1993).
5. Thompson et al. (1991). Finley, Ögelman, and Kiziloğlu (1992).
6. Halpern and Ruderman (1993).
7. Brinkmann and Ögelman (1987).
8. Ögelman and Finley (1993). Anderson et al. (1993).