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Scatter plot showing energy in mega electron-volts vs. relative time in seconds for three neutrino detectors: Kamiokande II (red points), IMB (green points) and Baksan (red points). The energy values on the y-axis range from 0 to 50 mega electron-volts. The time values on the x-axis range from 0 to 14 seconds. The data is shown as dots with vertical error bars. The overall trend shows a peak between 0 and 2 seconds, with energies between 10 and 40 mega electron-volts. The points then slope downward from 4 to 14 seconds, with energies going from 20 to 10 mega electron-volts.

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Scatter plot showing energy in mega electron-volts vs. relative time in seconds for three neutrino detectors: Kamiokande II (red points), IMB (green points) and Baksan (red points). The energy values on the y-axis range from 0 to 50 mega electron-volts. The time values on the x-axis range from 0 to 14 seconds. The data is shown as dots with vertical error bars. The overall trend shows a peak between 0 and 2 seconds, with energies between 10 and 40 mega electron-volts. The points then slope downward from 4 to 14 seconds, with energies going from 20 to 10 mega electron-volts.
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Kelly Lepo (kellylepo@astrodon.social)'s status on Saturday, 02-Sep-2023 07:07:32 JST Kelly Lepo
in reply to

@morganism During a supernova, the core will collapse until it reaches nuclear densities. At this point, material will continue to fall in, producing a shock that propagates outward — the bounce. This shock releases a burst of subatomic particles known as neutrinos. The energy of the neutrinos tells us about the physics of the bounce.
Before the light from SN 1987A arrived, several neutrino detectors on Earth observed such a burst, in agreement with models.
Fig from: https://doi.org/10.1007/978-3-319-96854-4_12

In conversation about a year ago from astrodon.social permalink