581 research outputs found
Neutronization During Type Ia Supernova Simmering
Prior to the incineration of a white dwarf (WD) that makes a Type Ia
supernova (SN Ia), the star "simmers" for ~1000 years in a convecting, carbon
burning region. We have found that weak interactions during this time increase
the neutron excess by an amount that depends on the total quantity of carbon
burned prior to the explosion. This contribution is in addition to the
metallicity (Z) dependent neutronization through the 22Ne abundance (as studied
by Timmes, Brown, & Truran). The main consequence is that we expect a floor to
the level of neutronization that dominates over the metallicity contribution
when Z/Z_\odot<2/3, and it can be important for even larger metallicities if
substantial energy is lost to neutrinos via the convective Urca process. This
would mask any correlations between SN Ia properties and galactic environments
at low metallicities. In addition, we show that recent observations of the
dependences of SNe Ia on galactic environments make it clear that metallicity
alone cannot provide for the full observed diversity of events.Comment: Accepted for publication in The Astrophysical Journal, 5 pages, 4
figure
The Energy Dependence of Neutron Star Surface Modes and X-ray Burst Oscillations
We calculate the photon energy dependence of the pulsed amplitude of neutron
star (NS) surface modes. Simple approximations demonstrate that it depends most
strongly on the bursting NS surface temperature. This result compares well with
full integrations that include Doppler shifts from rotation and general
relativistic corrections to photon propagation. We show that the energy
dependence of type I X-ray burst oscillations agrees with that of a surface
mode, lending further support to the hypothesis that they originate from
surface waves. The energy dependence of the pulsed emission is rather
insensitive to the NS inclination, mass and radius, or type of mode, thus
hindering constraints on these parameters. We also show that, for this
energy-amplitude relation, the majority of the signal (relative to the noise)
comes in the 2-25 keV band, so that the current burst oscillation searches with
the Rossi X-Ray Timing Explorer are close to optimal. The critical test of the
mode hypothesis for X-ray burst oscillations would be a measurement of the
energy dependence of burst oscillations from an accreting millisecond pulsar.Comment: Accepted for publication in The Astrophysical Journal, 6 pages, 5
figures (revised version: no changes to text, just edited author list
The Turbulent Story of X-ray Bursts: Effects of Shear Mixing on Accreting Neutron Stars
During accretion, a neutron star (NS) is spun up as angular momentum is
transported through its liquid surface layers. We study the resulting
differentially rotating profile, focusing on the impact this has for type I
X-ray bursts. The viscous heating is found to be negligible, but turbulent
mixing can be activated. Mixing has the greatest impact when the buoyancy at
the compositional discontinuity between accreted matter and ashes is overcome.
This occurs preferentially at high accretion rates or low spin frequencies and
may depend on the ash composition from the previous burst. We then find two new
regimes of burning. The first is ignition in a layer containing a mixture of
heavier elements with recurrence times as short as ~5-30 minutes, similar to
short recurrence time bursts. When mixing is sufficiently strong, a second
regime is found where accreted helium mixes deep enough to burn stably,
quenching X-ray bursts altogether. The carbon-rich material produced by stable
helium burning would be important for triggering and fueling superbursts.Comment: 3 pages, 3 figures. To appear in the proceedings of "Forty Years of
Pulsars: Millisecond Pulsars, Magnetars and More" held in Montreal, Canada,
August 12-17, 200
Thermonuclear burst physics with RXTE
Recently we have made measurements of thermonuclear burst energetics and
recurrence times which are unprecedented in their precision, largely thanks to
the sensitivity of the Rossi X-ray Timing Explorer. In the "Clocked Burster",
GS 1826-24, hydrogen burns during the burst via the rapid-proton (rp) process,
which has received particular attention in recent years through theoretical and
modelling studies. The burst energies and the measured variation of alpha (the
ratio of persistent to burst flux) with accretion rate strongly suggests solar
metallicity in the neutron star atmosphere, although this is not consistent
with the corresponding variation of the recurrence time. Possible explanations
include extra heating between the bursts, or a change in the fraction of the
neutron star over which accretion takes place. I also present results from 4U
1746-37, which exhibits regular burst trains which are interrupted by "out of
phase" bursts.Comment: 4 pages, 2 figures, AIP conference proceedings format. To appear in
the proceedings of the "X-ray Timing 2003: Rossi and Beyond" meeting held in
Cambridge, MA, November, 200
Ignition column depths of helium-rich thermonuclear bursts from 4U 1728-34
We analysed thermonuclear (type-I) X-ray bursts observed from the low-mass
X-ray binary 4U1728-34 by RXTE, Chandra and INTEGRAL. We compared the variation
in burst energy and recurrence times as a function of accretion rate with the
predictions of a numerical ignition model including a treatment of the heating
and cooling in the crust. We found that the measured burst ignition column
depths are significantly below the theoretically predicted values, regardless
of the assumed thermal structure of the neutron star interior. While it is
possible that the accretion rate measured by Chandra is underestimated, due to
additional persistent spectral components outside the sensitivity band, the
required correction factor is typically 3.6 and as high as 6, which is
implausible. Furthermore, such underestimation is even more unlikely for RXTE
and INTEGRAL, which have much broader bandpasses. Possible explanations for the
observed discrepancy include shear-triggered mixing of the accreted helium to
larger column depths, resulting in earlier ignition, or the fractional covering
of the accreted fuel on the neutron star surface.Comment: 12 pages, 5 figures, accepted for publication in Ap
A numerical study of the r-mode instability of rapidly rotating nascent neutron stars
The first results of numerical analysis of classical r-modes of {\it rapidly}
rotating compressible stellar models are reported. The full set of linear
perturbation equations of rotating stars in Newtonian gravity are numerically
solved without the slow rotation approximation. A critical curve of
gravitational wave emission induced instability which restricts the rotational
frequencies of hot young neutron stars is obtained. Taking the standard cooling
mechanisms of neutron stars into account, we also show the `evolutionary
curves' along which neutron stars are supposed to evolve as cooling and
spinning-down proceed. Rotational frequencies of stars suffering
from this instability decrease to around 100Hz when the standard cooling
mechanism of neutron stars is employed. This result confirms the results of
other authors who adopted the slow rotation approximation.Comment: 4 pages, 2 figures; MNRAS,316,L1(2000
Rotational Broadening of Atomic Spectral Features from Neutron Stars
The discovery of the first gravitationally redshifted spectral line from a
neutron star (NS) by Cottam, Paerels and Mendez has triggered theoretical
studies of the physics of atomic line formation in NS atmospheres. Chang,
Bildsten and Wasserman showed that the hydrogenic Fe H line formed
above the photosphere of a bursting NS is intrinsically broad. We now include
rotational broadening within general relativity and compare the resulting
profile to that observed during Type I bursts from EXO 0748-676. We show that
the fine structure splitting of the line precludes a meaningful constraint on
the radius. Our fitting of the data show that the line forming Fe column is
and
gravitational redshift with 95% confidence. We
calculate the detectability of this spectral feature for a large range of spins
and inclinations assuming that the emission comes from the entire surface. We
find that at 300 (600) Hz only 10-20% (5-10%) of NSs would have spectral
features as deep as that seen in EXO 0748-676.Comment: 4 pages, 4 figures, to appear in ApJ Letter
The ERP System for an Effective Management of a Small Software Company – Requirements Analysis
As found out by a questionnaire survey a significant part of small software companies is not satisfied with the way their company processes are supported by software systems. To change this situation it is necessary first to specify requirements for such software systems in small software companies. Based on the analysis of the literature and the market and own experience the first version of the ERP system requirements specification for small software companies was framed and subsequently validated by interviewing the executives of the target group companies
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