the first cosmic explosions
DESCRIPTION
The First Cosmic Explosions. Daniel Whalen McWilliams Fellow Carnegie Mellon University Chris Fryer, Lucy Frey LANL Candace Joggerst UCSC/LANL. ~ 200 pc. Cosmological Halo z ~ 20. Transformation of the Halo Whalen, Abel & Norman 2004, ApJ, 610, 14. Chemical Mixing Prior to Breakout. - PowerPoint PPT PresentationTRANSCRIPT
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The First Cosmic Explosions
Daniel WhalenMcWilliams Fellow Carnegie Mellon University
Chris Fryer, Lucy FreyLANL
Candace Joggerst UCSC/LANL
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~ 200 pc
CosmologicalHalo z ~ 20
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Transformation of the HaloWhalen, Abel & Norman 2004, ApJ, 610, 14
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Chemical Mixing Prior to Breakout
Joggerst & Whalen 2010, ApJ in prep
PISNCore Collapse SN
Joggerst, Whalen, et al 2010, ApJ, 709, 11
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Reverse Shock Collision with the Shell
Primordial SNe in Relic H II RegionsWhalen, Van Veelen, O’Shea & Norman ApJ 2008, 682,49
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Late Radiative Phase Fallback
Primordial SNe in Neutral Halos
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Conclusions I
• elemental yields of primordial SNe depend on both explosive nucleosynthesis and mixing and fallback within the star
• metals mix with primordial gas on 3 characteristic spatial scales in primordial SNe (inside the star, 10 - 15 pc and 100 - 200 pc)
• Salpeter-type IMF averages of 15 - 40 solar mass Pop III core-collapse SNe are the best fit to EMP star abundances thus far, although considerable work remains
• metal and dust cooling in Pop III SNe remnants may lead to prompt second star formation
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LANL Pop III Supernova Light Curve EffortWhalen, Fryer & Frey, ApJ 2010a,b, in prep
• LANL ASC code RAGE (Radiation Adaptive Grid Eulerian)
• 1D RTP AMR radiation hydrodynamics with grey/multigroup FLD and Implicit Monte Carlo transport
• 2T models (radiation and matter not assumed to be at the same temperature)
• PISN, core-collapse, and hypernova models
• post process rad hydro profiles to obtain spectra and light curves
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Post Processing Includes Detailed LANL Opacities
but the atomic levels areassumed to be in equilibrium,a clear approximation
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PISN Shock Breakout
• X-rays (< 1 keV)
• transient (a few hours in the local frame)
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Spectra atBreakout
The spectra evolverapidly as the frontcools
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Long-Term Light Curve Evolution
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Late Time Spectra
spectral features after breakout may enable usto distinguish betweenPISN and CC SNe
larger parameter studywith well-resolved photospheres is now inprogress
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Roadmap Ahead
• current models are grey FLD; next step is multigroup FLD and then multigroup IMC
• advance from 1D RTP AMR calculations to 2D cartesian AMR grids
• incorporate mixing from 2D models to simulate core-collapse SNe (15 - 40 solar mass stars, hypernovae)
• implement non-equilibrium opacities
• investigate progenitor environments on LC and spectra (LBV brightening?)
• explore asymmetric explosion mechanisms
• evolve toward 2D AMR IMC rad hydro with thousands of frequency bins -- eliminate post processing
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Conclusions II
• PISN will be visible to JWST out to z ~ 10 - 15; strong lensing may enable their detection out to z ~ 20 (Holz, Whalen & Fryer 2010 ApJ in prep)
• dedicated ground-based followup with 30-meter class telescopes for primordial SNe spectroscopy
• discrimination between Pop III PISN and Pop III CC SNe will be challenging but offers the first direct constraints on the Pop III IMF
• complementary detection of Pop III PISN remnants by the SZ effect may be possible (Whalen, Bhattacharya & Holz 2010, ApJ in prep)