scholarly journals Sensitivity of Type I X-Ray Bursts to rp-Process Reaction Rates

2010 ◽  
Author(s):  
A. Matthew Amthor ◽  
Daniel Galaviz ◽  
Alexander Heger ◽  
Alexander Sakharuk ◽  
Hendrik Schatz ◽  
...  
Keyword(s):  
Reaction Rates ◽  
Type I ◽  
X Ray ◽  
Rp Process

scholarly journals Urca nuclide production in Type-I X-ray bursts and implications for nuclear physics studies

2020 ◽  
Vol 500 (3) ◽  
pp. 2958-2968
Author(s):  
Grant Merz ◽  
Zach Meisel
Keyword(s):  
Light Curve ◽  
Nuclear Reaction ◽  
Nuclear Physics ◽  
Thermal Structure ◽  
Reaction Rates ◽  
High Mass ◽  
Type I ◽  
Model Calculations ◽  
X Ray ◽  
Lower Temperature

ABSTRACT The thermal structure of accreting neutron stars is affected by the presence of urca nuclei in the neutron star crust. Nuclear isobars harbouring urca nuclides can be produced in the ashes of Type I X-ray bursts, but the details of their production have not yet been explored. Using the code MESA, we investigate urca nuclide production in a one-dimensional model of Type I X-ray bursts using astrophysical conditions thought to resemble the source GS 1826-24. We find that high-mass (A ≥ 55) urca nuclei are primarily produced late in the X-ray burst, during hydrogen-burning freeze-out that corresponds to the tail of the burst light curve. The ∼0.4–0.6 GK temperature relevant for the nucleosynthesis of these urca nuclides is much lower than the ∼1 GK temperature most relevant for X-ray burst light curve impacts by nuclear reaction rates involving high-mass nuclides. The latter temperature is often assumed for nuclear physics studies. Therefore, our findings alter the excitation energy range of interest in compound nuclei for nuclear physics studies of urca nuclide production. We demonstrate that for some cases this will need to be considered in planning for nuclear physics experiments. Additionally, we show that the lower temperature range for urca nuclide production explains why variations of some nuclear reaction rates in model calculations impacts the burst light curve but not local features of the burst ashes.

scholarly journals New Reaction Rates Of 64Ge(p,γ)65As(p,γ)66Se And The Impact On Type I X-ray Bursts

2017 ◽  
Author(s):  
Yi Hua Lam ◽  
Jianjun He ◽  
Hendrik Schatz ◽  
B. Alex Brown ◽  
Anuj Parikh
Keyword(s):  
Reaction Rates ◽  
Type I ◽  
X Ray ◽  
The Impact

scholarly journals New thermonuclear reaction rates of64Ge(p,γ)65As and65As(p,γ)66Se for type-I x-ray bursts

2016 ◽  
Vol 109 ◽  
pp. 05005
Author(s):  
Yi Hua Lam ◽  
Jianjun He ◽  
Anuj Parikh ◽  
B. Alex Brown
Keyword(s):  
Reaction Rates ◽  
Type I ◽  
Thermonuclear Reaction ◽  
X Ray

scholarly journals Models of Type I X-Ray Bursts from GS 1826-24: A Probe of rp-Process Hydrogen Burning

2007 ◽  
Vol 671 (2) ◽  
pp. L141-L144 ◽  
Author(s):  
Alexander Heger ◽  
Andrew Cumming ◽  
Duncan K. Galloway ◽  
Stanford E. Woosley
Keyword(s):  
Type I ◽  
Hydrogen Burning ◽  
X Ray ◽  
Rp Process

scholarly journals White Dwarf Models of Supernovae and Cataclysmic Variables

1987 ◽  
Vol 93 ◽  
pp. 395-411
Author(s):  
K. Nomoto ◽  
M. Hashimoto
Keyword(s):  
White Dwarf ◽  
White Dwarfs ◽  
Cataclysmic Variables ◽  
Reaction Rates ◽  
Type I ◽  
X Ray ◽  
Composition Structure ◽  
Helium Star ◽  
X Ray Binaries ◽  
Good Agreement

AbstractIf the accreting white dwarf increases its mass to the Chandrasekhar mass, it will either explode as a Type I supernova or collapse to form a neutron star. In fact, there is a good agreement between the exploding white dwarf model for Type I supernovae and observations. We describe various types of evolution of accreting white dwarfs as a function of binary parameters (i.e, composition, mass, and age of the white dwarf, its companion star, and mass accretion rate), and discuss the conditions for the precursors of exploding or collapsing white dwarfs, and their relevance to cataclysmic variables. Particular attention is given to helium star cataclysmics which might be the precursors of some Type I supernovae or ultrashort period X-ray binaries. Finally we present new evolutionary calculations using the updated nuclear reaction rates for the formation of O+Ne+Mg white dwarfs, and discuss the composition structure and their relevance to the model for neon novae.

scholarly journals REACTION RATES OF64Ge(p,γ)65As AND65As(p,γ)66Se AND THE EXTENT OF NUCLEOSYNTHESIS IN TYPE I X-RAY BURSTS

2016 ◽  
Vol 818 (1) ◽  
pp. 78 ◽  
Author(s):  
Y. H. Lam ◽  
J. J. He ◽  
A. Parikh ◽  
H. Schatz ◽  
B. A. Brown ◽  
...  
Keyword(s):  
Reaction Rates ◽  
Type I ◽  
X Ray

scholarly journals The study of multipeaked type-I X-ray bursts in the neutron star low-mass X-ray binary 4U 1636 − 536 with RXTE

2020 ◽  
Vol 501 (1) ◽  
pp. 168-178
Author(s):  
Chen Li ◽  
Guobao Zhang ◽  
Mariano Méndez ◽  
Jiancheng Wang ◽  
Ming Lyu
Keyword(s):  
Neutron Star ◽  
Flux Ratio ◽  
Light Curves ◽  
Type I ◽  
X Ray ◽  
Soft State ◽  
Peak Flux ◽  
Low Mass ◽  
Two Peaks ◽  
Second Peak

ABSTRACT We have found and analysed 16 multipeaked type-I bursts from the neutron-star low-mass X-ray binary 4U 1636 − 53 with the Rossi X-ray Timing Explorer (RXTE). One of the bursts is a rare quadruple-peaked burst that was not previously reported. All 16 bursts show a multipeaked structure not only in the X-ray light curves but also in the bolometric light curves. Most of the multipeaked bursts appear in observations during the transition from the hard to the soft state in the colour–colour diagram. We find an anticorrelation between the second peak flux and the separation time between two peaks. We also find that in the double-peaked bursts the peak-flux ratio and the temperature of the thermal component in the pre-burst spectra are correlated. This indicates that the double-peaked structure in the light curve of the bursts may be affected by enhanced accretion rate in the disc, or increased temperature of the neutron star.

Latitudinal Shear Instabilities during Type I X‐Ray Bursts

2005 ◽  
Vol 630 (1) ◽  
pp. 441-453 ◽  
Author(s):  
Andrew Cumming
Keyword(s):  
Type I ◽  
X Ray ◽  
Shear Instabilities
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