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Brown Dwarf Desert Project: Second Presentation

Brown Dwarf Desert Project: Second Presentation. Peter Jumper. Results. Ultimately inconclusive this semester Have been deadlocked for some time. The Problem. When we ran the code, we got NaN values Occurs even during the test of a simplified case, a rigid, rotating body

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Brown Dwarf Desert Project: Second Presentation

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  1. Brown Dwarf Desert Project: Second Presentation Peter Jumper

  2. Results • Ultimately inconclusive this semester • Have been deadlocked for some time

  3. The Problem • When we ran the code, we got NaN values • Occurs even during the test of a simplified case, a rigid, rotating body • Affects period, semimajor axis, and specific angular momentum outputs • Module testing will be critical

  4. Using a Debugger • Dr. Fisher suggested this • In principle, this should be greatly helpful • I have experience using debuggers in ECE 160 • I have never run a debugger on the command line, however • My efforts to run the debugger have been unsuccessful

  5. Plans to Solve the Problem • Participation in CSUMS program during the summer

  6. Conferences • Prepared presentation and poster on my work • Presented at four conferences during April (SPS, APS-AAPT, Sigma Xi, Massachusetts Statewide Undergraduate Research Conference) • These conferences provided valuable experience

  7. My Presentation

  8. Shaping the Brown Dwarf Desert: Constraints fromTurbulent Fragmentation Dr. Robert T. Fisher, Peter Jumper, and DeividRibeiro

  9. What is the Brown Dwarf Desert? • The notable absence of brown dwarfs within five times the Earth-Sun distance from their central star (Grether and Lineweaver 2004)

  10. Why Do We Care? • Improve understanding of angular momentum transfer in the star formation process • Scaled-up planets? • Scaled-down stars?

  11. Past Research • Brown dwarfs migrating into the central stars proposed Credit: Phil Armitage

  12. Gravitational Fragmentation Model • Core: star-forming gaseous cloud • Models deal with the formation of two stars from the core • Mass and angular momentum of stars dependent on the core ε* = (M1 + M2)/Mcore εJ = J/Jcore

  13. Turbulent Fragmentation • Core angular momentum comes from turbulence • Net angular momentum is nonzero Credit: (Seinfeld 1986)

  14. Methodology • Draw masses from the initial mass function • Gaussian random field gives turbulence and angular momentum • Calculate orbital parameters

  15. Research Progress • Conducting verification by reproducing results of an earlier paper • Troubleshooting • New initial mass function code prepared

  16. Future Plans • Conduct simulations for 200 brown dwarf – binary systems • Analysis of results

  17. Questions?

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