New Reaction Rates of 64 Ge(p,γ) 65 As and 65 As(p,γ) 66 Se and the Impact on Nucleosynthesis in Type-I X-ray Bursts
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1 New Reaction Rates of 64 Ge(p,γ) 65 As and 65 As(p,γ) 66 Se and the Impact on Nucleosynthesis in Type-I X-ray Bursts Yi Hua LAM ( 藍乙華 ) Collaborators: Jian Jun HE ( 何建軍 ), Anuj PARIKH, Hendrik SCHATZ, B. Alex BROWN, Meng WANG ( 王猛 ), Bing GUO ( 郭冰 ), Yu Hu ZHANG ( 張玉虎 ), Xiao Hong ZHOU ( 周小紅 ), Hu San XU ( 徐瑚珊 ) 中国科学院近代物理研究所 Institute of Modern Physics (IMP) Chinese Academy of Sciences (CAS) 2016 International Nuclear Physics Conference, Sept. 2016, Adelaide, Australia.
2 New Reaction Rates of 64 Ge(p,γ) 65 As and 65 As(p,γ) 66 Se and the Impact on Nucleosynthesis in Type-I X-ray Bursts Background Type-I x-ray burst (and models) Rapid-proton capture (rp) process New rp-process reaction rates of 64 Ge(p,γ) 65 As and 65 As(p,γ) 66 Se The impact on end-stage abundances and light curve Summary and Perspectives
3 Type I X-ray burst (XRB) Discovered independently by Belian+. (1976) and Grindlay+. (1976) The stellar binary system is close enough to permit mass transfer. The solar-type matter flow forms an accretion disk surrounding the neutron star and ultimately accumulates on its surface, building up an envelope in semi-degenerate conditions. Artistic image from David. A. Hardy / STFC As material piles up on top of the neutron star, the envelope is heated up without any significant expansion due to degeneracy, driving a violent thermonuclear runaway. 3/0
4 Type I X-ray burst (XRB) Discovered independently by Belian+. (1976) and Grindlay+. (1976) The stellar binary system is close enough to permit mass transfer. The solar-type matter flow forms an accretion disk surrounding the neutron star and ultimately accumulates on its surface, building up an envelope in semi-degenerate conditions. Artistic image from David. A. Hardy / STFC As material piles up on top of the neutron star, the envelope is heated up without any significant expansion due to degeneracy, driving a violent thermonuclear runaway. 4/0
5 Type I X-ray burst (XRB) Discovered independently by Belian+. (1976) and Grindlay+. (1976) The stellar binary system is close enough to permit mass transfer. The solar-type matter flow forms an accretion disk surrounding the neutron star and ultimately accumulates on its surface, building up an envelope in semi-degenerate conditions. Artistic image from David. A. Hardy / STFC As material piles up on top of the neutron star, the envelope is heated up without any significant expansion due to degeneracy, driving a violent thermonuclear runaway. 5/0
6 Type I X-ray burst (XRB) Reaching A>60 and even A>100 Burst energies: ergs; timescales: s; recurrence times: hours days; max. temperatures: 1 2 GK; densities: ~10 6 g/cm 3. Drive nucleosynthesis along the proton-rich side: rp process [(p, ) reactions ] (main process) p process [a sequence of (,p), (p, ) reactions ] 3 -reaction β + decay Parikh+ (2008, 2009, 2013), Woosley+(2004), Schatz+ (1999) 6/0
7 Type I X-ray burst (XRB) rapid proton capture (rp)-process Reaching A>60 and even A>100 Drive nucleosynthesis along the proton-rich side: rp process [(p, ) reactions ] (main process) p process [a sequence of (,p), (p, ) reactions ] 3 -reaction β + decay Artistic image from David. A. Hardy / STFC Parikh+ (2008, 2009, 2013), Woosley+(2004), Schatz+ (1999) Nuclear chart from Langanke & Schatz, Phys Scr T152 (2013) /0
8 Type I X-ray burst (XRB) rapid proton capture (rp)-process Reaching A>60 and even A>100 Burst energies: ergs; timescales: s; recurrence times: hours days; max. temperatures: 1 2 GK; densities: ~10 6 g/cm 3. Drive nucleosynthesis along the proton-rich side: rp process [(p, ) reactions ] (main process) p process [a sequence of (,p), (p, ) reactions ] 3 -reaction β + decay Artistic image from David. A. Hardy / STFC Parikh+ (2008, 2009, 2013), Woosley+(2004), Schatz+ (1999) Nuclear chart from Langanke & Schatz, Phys Scr T152 (2013) /0
9 Type I X-ray burst (XRB) rapid proton capture (rp)-process Drive nucleosynthesis along the proton-rich side: rp process [(p, ) reactions ] (main process) p process [a sequence of (,p), (p, ) reactions ] 3 -reaction β + decay Artistic image from David. A. Hardy / STFC Parikh+ (2008, 2009, 2013), Woosley+(2004), Schatz+ (1999) Nuclear chart from Langanke & Schatz, Phys Scr T152 (2013) /0
10 Type I X-ray burst (XRB) rapid proton capture (rp)-process waiting point p, γ γ, p, λ(β) small (p, ) Q-value : kt at XRB temperatures Drive nucleosynthesis along the proton-rich side: rp process [(p, ) reactions ] (main process) p process [a sequence of (,p), (p, ) reactions ] 3 -reaction β + decay Artistic image from David. A. Hardy / STFC Parikh+ (2008, 2009, 2013), Woosley+(2004), Schatz+ (1999) Nuclear chart from Langanke & Schatz, Phys Scr T152 (2013) /0
11 Type I X-ray burst (XRB) rapid proton capture (rp)-process 11/0
12 rapid proton capture (rp)-process 68 Se(p,γ) 69 Br Rogers+ J. Phys. Conf. Ser. 312 (2011) Sensitive to nucl. phys. input for waiting point: 64 Ge(p, ) 65 As(e + n) 65 Ge 64 Ge(p, ) 65 As(p, ) 66 Se(e + n) 66 As 65 As(p,γ) 66 Se 64 Ge(p,γ) 65 As impact on nucleosynthesis during XRBs Parikh+ (2014); (2009); (2008) Woosley+, ApJ Suppl 151 (2004) 75 Nuclear chart from Langanke & Schatz, Phys Scr T152 (2013) /0
13 rapid proton capture (rp)-process 68 Se(p,γ) 69 Br Rogers+ J. Phys. Conf. Ser. 312 (2011) Sensitive to nucl. phys. input for waiting point: 64 Ge(p, ) 65 As(e + n) 65 Ge 64 Ge(p, ) 65 As(p, ) 66 Se(e + n) 66 As waiting point 64 Ge Tu+ (2011) 65 As(p,γ) 66 Se 64 Ge(p,γ) 65 As waiting point: 64 Ge Schatz+ (1998); Woosley+ (2004); Fisker+ (2008); Parikh+ (2009); Jose+ (2010) Woosley+, ApJ Suppl 151 (2004) 75 Nuclear chart from Langanke & Schatz, Phys Scr T152 (2013) /0
14 Nuclear structure Large scale shell-model calculations + exp. data Experiment: Obertelli+ (2011), Ruotsalainen+(2013), NNDC Theory: Shell model (GXPF1a) Sp: AME(2012), Tu+ (2011) gamma width, Spectroscopic factor: θ 2 if = 1 2J + 1 φ f A 1 J a nlj φ A i J 2 14/0
15 Nuclear structure Large scale shell-model calculations + exp. data Experiment: Obertelli+ (2011), Ruotsalainen+(2013), NNDC Theory: Shell model (GXPF1a) Sp: AME(2013), Tu+ (2011) gamma width, Spectroscopic factor: θ 2 if = 1 2J + 1 φ f A 1 J a nlj φ A i J 2 15/0
16 Comparisons of present reaction rates with JINA data (REACLIB) rpsm (Sp=-0.081MeV) Audi & Wapstra (1995) rath (Sp= 0.128MeV) FDRM Rauscher & Thielemann (2000) thra (Sp= 1.399MeV) ETSFIQ laur (Sp= 0.169MeV) Van Wormer+ (1994) ths8 (Sp= 0.255MeV) Rauscher (Cyburt+ 2010) present work (Sp= / MeV) Exp. levels & Sp + evaluated mass + shell model 64 Ge(p,γ) 65 As 65 As(p,γ) 66 Se 16/0
17 Comparisons of reaction rates 64 Ge(p,γ) 65 As Hauser-Feshbach (statistical model) rates High density of excited states in 65 As Proton separation energy, S p ( 65 As) Upper limit Lower limit 17/0
18 Comparisons of reaction rates 65 As(p,γ) 66 Se Hauser-Feshbach (statistical model) rates may suffer from unknown systematic errors near proton drip line laur: Only 3 excited states Van Wormer+ (1994) Upper limit Lower limit 18/0
19 abundance (mole/g) Abundance distribution of the XRB ashes ratio = Abundance of A = 64 Abundance of A = 68 ratio = 1.1, 64 Ge the strongest waiting point ratio = 0.7, 64 Ge not a significant waiting point Upper limit Lower limit Present 64 Ge(p,γ) 65 As and 65 As(p,γ) 66 Se 19/0
20 abundance (mole/g) Abundances and end stage light curve A 106, heavy-isotope production is enhanced, slower burning at high T and leading to longer burst Upper limit Lower limit Present 64 Ge(p,γ) 65 As and 65 As(p,γ) 66 Se 20/0
21 abundance (mole/g) Abundances and end stage light curve A 106, heavy-isotope production is reduced, faster burning at high T consuming H quickly and leading to shorter burst Upper limit Lower limit Present 64 Ge(p,γ) 65 As and 65 As(p,γ) 66 Se 21/0
22 End stage light curve Changing only S p ( 65 As) and/or S p ( 66 Se): Producing (roughly) similar light curve Present 64 Ge(p,γ) 65 As and 65 As(p,γ) 66 Se 22/0
23 End stage light curve Changing only S p ( 65 As) and/or S p ( 66 Se): Producing (roughly) similar light curve Using nominal values of S p ( 65 As), S p ( 66 Se), and 64 Ge(p, ), vary 65 As(p, ) : Significant change of end light curve Abundance of A= ratio 1.0 Abundance of A=68 the 65 As(p, ) has significant role 65 As(p, ) upper limit 65 As(p, ) lower limit Present 64 Ge(p,γ) 65 As and 65 As(p,γ) 66 Se 23/0
24 Summary & Perspective New thermonuclear rates of 64 Ge(p,γ) 65 As and 65 As(p,γ) 66 Se reactions have been determined based on newly measured S p ( 65 As), evaluated S p ( 66 Se), largescale shell model calculation, and exp. levels of 65 As. These new rates differ, for instance at 1 GK, a factor of 3 90 from others. The waiting point 64 Ge is not completely ruled out using one-zone XRB model. We propose: to measure the mass of 66 Se, to obtain higher precision of mass 65 As, and nuclear structure of both nuclei investigation with 1D multi-zone hydrodynamic XRB model. 24/0
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