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Astronomy research
Software Infrastructure:
MESA
FLASH-X
STARLIB
MESA-Web
starkiller-astro
My instruments
White dwarf pulsations:
Probe of 12C(α,γ)16O
Impact of 22Ne
Impact of ν cooling
Variable white dwarfs
MC reaction rates
Micronovae
Novae
White dwarf supernova:
Stable nickel production
Remnant metallicities
Colliding white dwarfs
Merging white dwarfs
Ignition conditions
Metallicity effects
Central density effects
Detonation density
Tracer particle burning
Subsonic burning fronts
Supersonic fronts
W7 profiles
Massive stars:
Pop III with HST/JWST
Rotating progenitors
3D evolution to collapse
MC reaction rates
Pre-SN variations
Massive star supernova:
26Al & 60Fe
44Ti, 60Co & 56Ni
SN 1987A light curve
Constraints on Ni/Fe
An r-process
Effects of 12C +12C
Neutron Stars and Black Holes:
Black Hole spectrum
Mass Gap with LVK
Compact object IMF
He burn neutron stars
Neutrino Emission:
Identifying the Pre-SN
Neutrino HR diagram
Pre-SN Beta Processes
Pre-SN neutrinos
Stars:
Hypatia catalog
SAGB stars
Nugrid Yields I
He shell convection
BBFH at 40 years
γ-rays within 100 Mpc
Iron Pseudocarbynes
Pre-Solar Grains:
C-rich presolar grains
SiC Type U/C grains
Grains from massive stars
Placing the Sun
SiC Presolar grains
Chemical Evolution:
Zone models H to Zn
Mixing ejecta
Thermodynamics & Networks
Skye EOS
Helm EOS
Five EOSs
Equations of State
12C(α,γ)16O Rate
Proton-rich NSE
Reaction networks
Bayesian reaction rates
Verification Problems:
Validating an astro code
Su-Olson
Cog8
RMTV
Sedov
Noh
Software instruments
Presentations
Illustrations
Public Outreach
Education materials
2023 ASU Solar Systems Astronomy
2023 ASU Energy in Everyday Life

AAS Journals
2023 MESA VI
2023 MESA Marketplace
2023 MESA Classroom
2022 Earendel, A Highly Magnified Star
2022 White Dwarfs & 12C(α,γ)16O
2022 Black Hole Mass Spectrum
2022 MESA in Don't Look Up
2021 Bill Paxton, Tinsley Prize

Contact: F.X.Timmes
my one page vitae,
full vitae,
research statement, and
teaching statement.
Presupernova neutrinos: directional sensitivity and prospects for progenitor identification (2020)

In this article we explore the potential of current and future liquid scintillator neutrino detectors of $\mathcal O (10)$ kt mass to localize a pre-supernova neutrino signal in the sky. In the hours preceding the core collapse of a nearby star (at distance $D \lesssim$ 1 kpc), tens to hundreds of inverse beta decay events will be recorded, and their reconstructed topology in the detector can be used to estimate the direction to the star. Although the directionality of inverse beta decay is weak ($\sim$8% forward-backward asymmetry for currently available liquid scintillators), we find that for a fiducial signal of 200 events (which is realistic for Betelgeuse), a positional error of $\sim$60$^\circ$ can be achieved, resulting in the possibility to narrow the list of potential stellar candidates to less than ten, typically. For a configuration with improved forward-backward asymmetry ($\sim$40%, as expected for a lithium-loaded liquid scintillator), the angular sensitivity improves to $\sim$15$^\circ$, and -- when a distance upper limit is obtained from the overall event rate -- it is in principle possible to uniquely identify the progenitor star. Any localization information accompanying an early supernova alert will be useful to multi-messenger observations and to particle physics tests using collapsing stars.

 Number of events at a 17 kt liquid scintillator detector Cumulative number at a 17 kt liquid scintillator detector Nearby core collapse supernova candidates Mollweide projection of nearby core collapse supernova candidates. Geometry of inverse beta decay in liquid scintillator Angular uncertainty of localization Antares 4 hours before collapse Antares 1 hour before collapse Antares 2 min before collapse

Neutrinos from beta processes in a presupernova: probing the isotopic evolution of a massive star (2017)

In this article we present a new calculation of the neutrino flux received at Earth from a massive star in the $\sim$ 24 hours of evolution prior to its explosion as a supernova (presupernova). Using the stellar evolution code MESA, the neutrino emissivity in each flavor is calculated at many radial zones and time steps. In addition to thermal processes, neutrino production via beta processes is modeled in detail, using a network of 204 isotopes. We find that the total produced $\nu_e$ flux has a high energy spectrum tail, at E $\gtrsim$ 3 - 4 MeV, which is mostly due to decay and electron capture on isotopes with A = 50 - 60. In a tentative window of observability of E $\gtrsim$ 0.5 MeV and t < 2 hours pre-collapse, the contribution of beta processes to the $\nu_e$ flux is at the level of $\sim$ 90% . For a star at D=1 kpc distance, a 17 kt liquid scintillator detector would typically observe several tens of events from a presupernova, of which up to $\sim$ 30% due to beta processes. These processes dominate the signal at a liquid argon detector, thus greatly enhancing its sensitivity to a presupernova.

 neutrino luminosity evolutions neutrino spectra $\nu$ luminosity evolution at different energies fluxes at earth for 15 M$_{\odot}$ fluxes at earth for 30 M$_{\odot}$