119 research outputs found
A Spallation Model for the Titanium-rich Supernova Remnant Cassiopeia A
Titanium-rich subluminous supernovae are rare and challenge current SN
nucleosynthesis models. We present a model in which ejecta from a standard
Supernova is impacted by a second explosion of the neutron star (a Quark-nova),
resulting in spallation reactions that lead to 56Ni destruction and 44Ti
creation under the right conditions. Basic calculations of the spallation
products shows that a delay between the two explosions of ~ 5 days reproduces
the observed abundance of 44Ti in Cas A and explains its low luminosity as a
result of the destruction of 56Ni. Our results could have important
implications for lightcurves of subluminous as well as superluminous
supernovae.Comment: Accepted/to be published in Physical Review Letters. [ for more info
on the Quark Nova, see: http://quarknova.ucalgary.ca/
Quark nova imprint in the extreme supernova explosion SN 2006gy
The extremely luminous supernova 2006gy (SN 2006gy) is among the most
energetic ever observed. The peak brightness was 100 times that of a typical
supernova and it spent an unheard of 250 days at magnitude -19 or brighter.
Efforts to describe SN 2006gy have pushed the boundaries of current supernova
theory. In this work we aspire to simultaneously reproduce the photometric and
spectroscopic observations of SN 2006gy using a quark nova model. This analysis
considers the supernova explosion of a massive star followed days later by the
quark nova detonation of a neutron star. We lay out a detailed model of the
interaction between the supernova envelope and the quark nova ejecta paying
special attention to a mixing region which forms at the inner edge of the
supernova envelope. This model is then fit to photometric and spectroscopic
observations of SN 2006gy. This QN model naturally describes several features
of SN 2006gy including the late stage light curve plateau, the broad H{\alpha}
line and the peculiar blue H{\alpha} absorption. We find that a progenitor mass
between 20Msun and 40Msun provides ample energy to power SN 2006gy in the
context of a QN.Comment: 15 pages, 9 figure
r-Java 2.0: the nuclear physics
[Aims:] We present r-Java 2.0, a nucleosynthesis code for open use that
performs r-process calculations as well as a suite of other analysis tools.
[Methods:] Equipped with a straightforward graphical user interface, r-Java 2.0
is capable of; simulating nuclear statistical equilibrium (NSE), calculating
r-process abundances for a wide range of input parameters and astrophysical
environments, computing the mass fragmentation from neutron-induced fission as
well as the study of individual nucleosynthesis processes. [Results:] In this
paper we discuss enhancements made to this version of r-Java, paramount of
which is the ability to solve the full reaction network. The sophisticated
fission methodology incorporated into r-Java 2.0 which includes three fission
channels (beta-delayed, neutron-induced and spontaneous fission) as well as
computation of the mass fragmentation is compared to the upper limit on mass
fission approximation. The effects of including beta-delayed neutron emission
on r-process yield is studied. The role of coulomb interactions in NSE
abundances is shown to be significant, supporting previous findings. A
comparative analysis was undertaken during the development of r-Java 2.0
whereby we reproduced the results found in literature from three other
r-process codes. This code is capable of simulating the physical environment
of; the high-entropy wind around a proto-neutron star, the ejecta from a
neutron star merger or the relativistic ejecta from a quark nova. As well the
users of r-Java 2.0 are given the freedom to define a custom environment. This
software provides an even platform for comparison of different proposed
r-process sites and is available for download from the website of the
Quark-Nova Project: http://quarknova.ucalgary.ca/Comment: 26 pages, 18 figures, 1 tabl
Deuterium burning in Jupiter interior
We show that moderate deviations from the Maxwell-Boltzmann energy
distribution can increase deuterium reaction rates enough to contribute to the
heating of Jupiter. These deviations are compatible with the violation of
extensivity expected from temperature and density conditions inside Jupiter.Comment: 6 pages, use elsart + 1 encaspulated postscript figure. Submitted to
Physica
Quark deconfinement in neutron star cores: The effects of spin-down
We study the role of spin-down in driving quark deconfinement in the high
density core of isolated neutron stars. Assuming spin-down to be solely due to
magnetic braking, we obtain typical timescales to quark deconfinement for
neutron stars that are born with Keplerian frequencies. Employing different
equations of state (EOS), we determine the minimum and maximum neutron star
masses that will allow for deconfinement via spin-down only. We find that the
time to reach deconfinement is strongly dependent on the magnetic field and
that this time is least for EOS that support the largest minimum mass at zero
spin, unless rotational effects on stellar structure are large. For a fiducial
critical density of for the transition to the quark phase
(g/cm is the saturation density of nuclear
matter), we find that neutron stars lighter than cannot reach a
deconfined phase. Depending on the EOS, neutron stars of more than
can enter a quark phase only if they are spinning faster than
about 3 milliseconds as observed now, whereas larger spin periods imply that
they are either already quark stars or will never become one.Comment: 4 pages, 4 figures, submitted to ApJ
Quark-Nova
We explore the scenario where the core of a neutron star (having experienced
a transition to an up and down quark phase) shrinks into the equilibrated quark
object after reaching strange quark matter saturation density (where a
composition of up, down and strange quarks is the favored state of matter). The
overlaying (envelope) material free-falls following the core contraction
releasing upto 10^{53} {\rm ergs} in energy as radiation, partly as a result of
the conversion of envelope material to quarks. This phenomena, we named
Quark-Nova, leads to a wide variety of ejectae ranging form the Newtonian,
"dirty" to the ultra-relativistic fireball. The mass range of the corresponding
compact remnant (the quark star) ranges from less than 0.3M_{\odot} up to a
solar mass. We discuss the connection between Quark-Novae and Gamma ray bursts
and suggest the recently studied GRB011211 event as a plausible Quark-Nova
candidate.Comment: 4 pages, 2 figures, shortened title. Major changes in the text,
version to appear in Astronomy&Astrophysic
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