主要内容:
精彩摘抄:
文章信息:
-
- · arXiv e-print (arXiv:1307.2943)
- · References in the Article
- · Citations to the Article (17) (Citation History)
- · Refereed Citations to the Article
- · Also-Read Articles (Reads History)
- ·
- · Translate This Page
| Title: |
| The long-term evolution of neutron star merger remnants - II. Radioactively powered transients |
| Authors: |
| Grossman, Doron; Korobkin, Oleg; Rosswog, Stephan; Piran, Tsvi |
| Publication: |
| eprint arXiv:1307.2943 |
| Publication Date: |
| 07/2013 |
| Origin: |
| ARXIV |
| Keywords: |
| Astrophysics - High Energy Astrophysical Phenomena |
| Comment: |
| 14 pages, 11 figures, 5 tables, accepted to MNRAS; doi:10.1093/mnras/stt2503 |
| Bibliographic Code: |
| 2013arXiv1307.2943G |
Abstract
We use 3D hydrodynamic simulations of the long-term evolution of neutron
star merger
ejecta to predict the light curves of electromagnetic
transients that are powered by the decay of freshly produced r-process
nuclei. For the dynamic
ejecta that are launched by tidal and
hydrodynamic interaction, we adopt
grey opacities of 10 cm$^2$/g, as
suggested by recent studies. For our reference case of a 1.3-1.4
$M_\odot$ merger, we find a broad IR peak 2-4 d after the merger. The
peak luminosity is $\approx 2\times 10^
{40
}$ erg/s for an average
orientation, but increased by up to a factor of 4 for more
favourable
binary parameters and viewing angles. These signals are rather weak and
hardly detectable within the large error box (~100 deg$^2$) of a
gravitational wave trigger. A second electromagnetic transient results
from neutrino-driven winds. These winds produce
`weak' r-process
material with $50 <
A < 130$ and abundance patterns that vary
substantially between different merger cases. For an adopted opacity of
1 cm$^2$/g, the resulting
transients peak in the UV/optical about 6 h
after the merger with a luminosity of $\approx 10^
{41
}$ erg/s (for a
wind of 0.01 $M_\odot$) These signals are marginally detectable in deep
follow-up searches (e.g.
using Hypersuprime camera on Subaru). A
subsequent detection of the
weaker but longer lasting IR signal would
allow an identification of the merger event. We briefly discuss the
implications of our results
to the recent detection of an
nIR transient
accompanying GRB 130603B.
