1 / 17

Impact of Nuclear Input on X-ray bursts

Richard H. Cyburt Ryan Ferguson Zach Meisel Scott Warren Matthew Amthor Karl Smith Hendrik Schatz. Impact of Nuclear Input on X-ray bursts. Outline. Motivation nuclear physics in astrophysics X-ray bursts Astrophysics in nuclear physics Conclusions. Motivation. nova.

novia
Download Presentation

Impact of Nuclear Input on X-ray bursts

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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

More Related