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Impact of Nuclear Input on X-ray Bursts in Astrophysics

Explore the influence of nuclear input on X-ray bursts in astrophysics, focusing on thermonuclear reactions, nuclear structure, and theoretical rates. Discover the implications for understanding neutron stars, nucleosynthesis, and elemental origins at SNP2008, Ohio University, July 8-11. Delve into the complexities of X-ray bursts, their characteristics, and the role of nuclear reactions. Uncover the significance of new theoretical reaction rates and database accessibility in advancing nuclear astrophysics. Join the discussion on leveraging X-ray bursts to enhance nuclear understanding and constrain exotic physics, while reflecting on the evolving landscape of nuclear astrophysics research.

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Impact of Nuclear Input on X-ray Bursts in Astrophysics

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  1. Richard H. Cyburt Ryan Ferguson Zach Meisel Scott Warren Matthew Amthor Karl SmithHendrik Schatz Impact of Nuclear Input onX-ray bursts SNP2008, Ohio University, July 8-11

  2. SNP2008, Ohio University, July 8-11 Outline Motivation nuclear physics in astrophysics X-ray bursts Astrophysics in nuclear physics Conclusions

  3. SNP2008, Ohio University, July 8-11 Motivation nova Big Bang Nucleosynthesis CR Nucleosynthesis supernova s-process x-ray bursts r-process stars p-process Origin of Elements! Explosion Light Curves!

  4. SNP2008, Ohio University, July 8-11 A Closer Look Nuclear Structure impacts nuclear astrophysics!

  5. SNP2008, Ohio University, July 8-11 Let’s consider X-ray bursts They’re explosions! They’re on neutron stars! They go off regularly! We can see ~1000s of them! Sounds pretty cool, but… How easy are they to understand?

  6. Type I X-ray bursts • Accreting H/He • but not too fast • n.s. fairly old • low B-field • slow rotation • Thermonuclear runaway SNP2008, Ohio University, July 8-11

  7. SNP2008, Ohio University, July 8-11 rp-process Helium burns to Carbon rapid (p,g)/(a,p)/+ decays Up the N=Z line on nuclide chart Peak brightness <A>~56

  8. SNP2008, Ohio University, July 8-11 Movie

  9. SNP2008, Ohio University, July 8-11 Nuclear input Thermonuclear reaction rates Not well covered by expt. Relies heavily on theory Which relies on nuclide masses weak decay rates Need  & T dependent rates Good expt. g.s. coverage Time lag incorporating new input

  10. SNP2008, Ohio University, July 8-11 rp-process db summary • expt based rates • thry based rates

  11. SNP2008, Ohio University, July 8-11 New Theory Rates (p,)‏ Within a factor of 2

  12. SNP2008, Ohio University, July 8-11 New Theory Rates (,p)‏

  13. SNP2008, Ohio University, July 8-11 Impact of New Rates

  14. SNP2008, Ohio University, July 8-11 Theory Rates Rates are all Rauscher rates Small impact w/ Rauscher rates What about other models? They need to be publically available!

  15. SNP2008, Ohio University, July 8-11 JINA Reaclib Database stores rxn rates in standard form remembers old versions Online interface easily accessible Provides link of communication

  16. SNP2008, Ohio University, July 8-11 www.nscl.msu.edu/~nero/db

  17. SNP2008, Ohio University, July 8-11 Conclusions Goal: nuke input not dom. uncertainty Use x-ray bursts to understand n.s. constrain exotic physics Nuclear astro. gaining much ground new expt. facilities/techniques large computational efforts Theories ever-scrutinized

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