¿Que viene después de una supernova?

Un resto de supernova o remanente de supernova (SNR por sus siglas en inglés) es la estructura nebulosa que resulta de la gigantesca explosión de una estrella como supernova.

¿Qué tipo de supernovas existen?

Existen dos tipos principales de supernovas: las gravitatorias y las termonucleares. Las supernovas gravitatorias (técnicamente, supernovas de tipos II, Ib, Ic) son explosiones que se producen al final de la vida de las estrellas muy masivas.

¿Qué es lo más grande que existe en el Universo?

TON 618 es un agujero negro ultramasivo cuya masa equivale a la de 66.000 millones de soles. Está a 18.000 millones de años luz de distancia, pero el disco de acreción que gira a su alrededor brilla con tanta fuerza (tanto como cien billones de estrellas) que podemos verlo desde la Tierra.

Are neutrinos produced in supernovae?

Supernovae are considered the strongest and most frequent source of cosmic neutrinos in the MeV energy range. Since neutrinos are generated in the core of a supernova, they play a crucial role in the star’s collapse and explosion. Neutrino heating is believed to be a critical factor in supernova explosions.

How much energy is carried away in a supernova?

An enormous amount of a supernova’s energy, a whopping 99 percent, is carried away by a burst of neutrinos (of all flavors) in a span of about 10 seconds. The core of the collapsing star is incredibly dense, but because neutrinos interact so rarely, they escape from the center even more quickly than the light does.

How many neutrinos did the supernova of SN 1987A capture?

In comparison, the supernova in 1987 (SN 1987A) resulted in 25 neutrino events captured across three detectors. Information from a supernova can be used to learn more about neutrinos, such as how they change over long distances and setting limits on how massive they can be.

What can we learn from supernovae?

Information from a supernova can be used to learn more about neutrinos, such as how they change over long distances and setting limits on how massive they can be. They can also be used to learn more about the life cycle of stars and the formation of neutron stars and black holes.