主要内容:
高红移的z~20的伽马暴的爆发simulation。说等红外仪器上天后可能可以测出红移从而确定。
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- · arXiv e-print (arXiv:1401.5565)
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Abstract
Gamma-ray bursts (GRBs) are the ultimate cosmic lighthouses, capable of
illuminating the universe at its earliest epochs. Could such events
probe the properties of the first stars at z $\sim$ 20, the end of the
cosmic Dark Ages? Previous studies of Population III GRBs only
considered explosions in the diffuse relic H II regions of their
progenitors, or bursts that are far
more more energetic than those
observed to date. But the processes that produce GRBs at the highest
redshifts likely reset their local environments, creating much more
complicated
structures than those in which relativistic jets have been
modeled so far. These structures can greatly affect the luminosity of
the afterglow, and hence the
redshift at which it can be detected. We
have now simulated Population III GRB afterglows in H II regions, winds,
and dense shells ejected by the star during the processes that produce
the
burst. Our model, which has been used in previous work, has been
extended to include contributions from reverse shocks, inverse Compton
cooling and the effects of
sphericity and beaming in the blast wave, and
is valid in a variety of
circumjet density profiles. We find that GRBs
with E$_{\mathrm{iso},\gamma} =$ 10$^
{ 51
}$ - 10$^
{53
}$ erg will be
visible at z $\gtrsim$ 20 to the next generation of near infrared and
radio observatories. In many cases, the environment of the burst, and
hence progenitor type, can be inferred from the afterglow light curve.
Although some Population III GRBs
are visible to Swift and the Very
Large Array now, the optimal strategy for their detection will be future
missions like EXIST and JANUS, which have large survey areas and
onboard
X-ray and infrared telescopes that can track their near infrared flux
from the moment of the burst, thereby identifying its
redshift.
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