Quasi-periodic X-ray oscillations in the source Scorpius X-1

Кузнецов, С. И.

doi:10.1134/1.1525832

Cited by 1 publication

(2 citation statements)

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“…GRB830801 is by far the all-time brightest GRB event known. With a peak flux of 3.0photons · cm −2 · s −1 · keV −1 averaged from 50 to 300 keV, a dead time correction by a factor of 1.9, and a smooth light curve for the peak 256 ms time interval (Kuznetsov et al 1986); the peak flux P 256 is around 1400photons · s −1 · cm −2 . For comparison, BATSE's brightest burst (GRB930131, the 'SuperBowl Burst') only has P 256 = 105photons·s −1 ·cm −2 .…”

Section: Grb 830801mentioning

confidence: 99%

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Redshifts and Luminosities for 112 Gamma-Ray Bursts

Schaefer

Deng

Band

2001

The Astrophysical Journal

124

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Two different luminosity indicators have recently been proposed for Gamma Ray Bursts that use gamma-ray observations alone. They relate the burst luminosity (L) with the time lag between peaks in hard and soft energies (τ lag ), and the spikiness or variability of the burst's light curve (V ). These relations are currently justified and calibrated with only 6 or 7 bursts with known red shifts. We have examined BATSE data for τ lag and V for 112 bursts. (1) A strong correlation between τ lag and V exists, and it is exactly as predicted from the two proposed relations. This is proof that both luminosity indicators are reliable.(2) GRB830801 is the all-time brightest burst, yet with a small V and a large τ lag , and hence is likely the closest known event being perhaps as close as 3.2 Mpc. (3) We have combined the luminosities as derived from both indicators as a means to improve the statistical and systematic accuracy when compared with the accuracy from either method alone. The result is a list of 112 bursts with good luminosities and hence red shifts. (4) The burst averaged hardness ratio rises strongly with the luminosity of the burst. (5) The burst luminosity function is a broken power law, with the break at L = 2 × 10 52 erg. The numbers in logarithmic bins scale as L −2.8±0.2 above the break and as L −1.7±0.1 below the break. (6) The number density of GRBs varies with red shift roughly as (1 + z) 2.5±0.3 between 0.2 < z < 5. This demonstrates that the burst rate follows the star formation rate at low red shifts, as expected since long bursts are generated by very massive stars. Excitingly, this result also provides a measure of the star formation rate out to z ∼ 5 with no effects from reddening, and the rate is rising uniformly for red shifts above 2.

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Section: Grb 830801mentioning

confidence: 99%

“…GRB830801 has a large lag. This can be quantified from Figure 4 of Kuznetsov et al (1986), from which the peak times of light curves can be read for seven energy bands. These peak times can be estimated to 0.25 s accuracy and plotted as a function of energy.…”

Section: Grb 830801mentioning

confidence: 99%