Presentation on theme: "Neutron Star Formation and the Supernova Engine Bounce Masses Mass at Explosion Fallback."— Presentation transcript:
Neutron Star Formation and the Supernova Engine Bounce Masses Mass at Explosion Fallback
Neutron Star Masses Observations of neutron star binaries provide a growing list of neutron star mass estimates. Current observations predict a range of NS masses from 1.0 to >2 solar masses. Can we explain these masses? Lattimer 2013
Neutrino-Driven Supernova Mechanism Temperature and Density of the Core Becomes so High that: Iron dissociates into alpha particles Electrons capture onto protons Core collapses nearly at freefall! Core reaches nuclear densities Nuclear forces and neutron degeneracy increase pressure Bounce! Radius (km) Velocity (c) Radius (km)
NS mass after the shock stalls Depends upon the entropy of the core. For Stars below ~15-20 solar masses, the stall is around 1.1 solar masses (using the latest MESA models).
The bounce depends upon the structure… Unfortunately this structure depends more on the stellar evolution code than it does on metallicity or progenitor mass. Total mass from stellar models: Heger Solar – 12.9 Heger Zero – 24.9 Limongi Zero – 24.7
Upflow Downflow Proto- Neutron Star Anatomy Of the Convection Region Fryer & Warren 2002 Accretion Shock We can derive the explosion energy from the duration of this phase! Fryer 2006 Neutrino-Driven Supernova Mechanism: Convective Phase
Binding Energy Of the Outer Layers Of the Star (M star -3 solar Masses) Fryer 1999
Anatomy of Fallback Fallback Mechanism Rarefaction wave: As the neutron star cools, it accretes, producing a rarefaction wave that catches the shock and decelerates it (Colgate 1971): Accretion happens quickly (first 100s) PdV work: The initial ejecta decelerates as it drives an explosion through the star. If the velocity decelerates below the escape velocity, it falls back (Fryer 1999): Accretion happens quickly (first 100s) Reverse shock: The shock decelerates in the flat density gradient of the envelope, driving a reverse shock. This decelerates the material behind the shock sufficiently to fall back (Nomoto 1988, Woosley 1988): Accretion takes 1000-10,000s.
Fallback rates It is difficult to avoid fallback. Most happens at early times, but at the level of 10 -4 Msun, this can happen even a year after the explosion.
Building a NS Atmosphere Free-fall Conditions Gamma-law EOS Radiation dominated Gas
Fallback Diagnostics - Nucleosynthesis Nuclear yields pervade many of the diagnostics discussed here (initial models, conditions for remnants) Detailed yields can also be compared to grains, stellar abundances, … r-process yields can also be used to constrain the conditions on the proto- neutron star (fallback, …) Fryer et al. 2006
Neutrinos from Fallback Neutrinos from cooling neutron stars emit below 1 foe/s at 10s with energies around 10MeV - Burrows 1988 Neutrinos from fallback are generally above 1 foe/s 5-10s after explosion with energies around 20 MeV – Fryer 2009
Moriya et al. 2010 Fallback Supernovae: a possible explanation for low energy supernovae
BH systems may place constraints on fallback. In the best observed systems, there exists an apparent gap in black hole masses from 3-5 M sun. Ozel et al. 2010 argue this gap is real! The gap argues for prompt explosions or some method to prevent fallback. But is this just an observational bias?
Compact Remnants The masses of compact remnants can be measured in binary systems (e.g. binary pulsar systems and X-ray binaries) and these observations are producing a growing list of masses. Advanced LIGO could dramatically increase these mass estimates
Gravitational mass determined by bounce – 1.0- 1.5 solar masses Gravitational mass determined by engine depends on the delay (the explosion energy is an indicator). Fallback typically adds another >0.1 solar masses of material. We can not match all the observations (the observations seem contradictory). BNS mergers provide a potential probe if we can distinguish NS from BH collapse systems. Conclusions
There are also issues with low-mass NSs The e-process (explosive burning of neutron- rich material – stellar cores will be neutron rich) will produce a lot of intermediate-mass elements. To avoid this, scientists have argued that all this must remain in the remnant. Unfortunately, if this occurs, we can’t make 1.0 solar mass neutron stars.
Atmosphere Extent The fallback atmosphere keeps expanding until neutrino cooling halts the expansion. This derivation assumes that the unstable entropy profile drives quick (and smooth) convection that equalizes the entropy. Energy Conservation Pair annihilation neutrino emission