Title: On the Nature of Rapidly Fading Type II Supernovae
Authors: Takashi J. Moriya, Maria V. Pruzhinskaya, Mattias Ergon and Sergei I. Blinnikov
First Author’s Institution: University of Bonn
Status: Accepted to MNRAS
The most luminous cosmic explosions come from the violent deaths of stars or supernovae. There is plenty of diversity among stars, so it’s not surprise that supernovae are also extremely diverse. The supernovae medley can arise from differences in the progenitor stars’ lives, environments or final moments.
Type II supernovae are those who show signs of hydrogen atoms. We see these atoms because the star takes on a “onion” profile before it collapses. In other words, the lighter elements (like hydrogen and helium) lie in outer shells of the star, while heavier elements (like iron and silicon) lie close to its core, like you can see in Figure 1.
It turns out that this layer of hydrogen has a big effect on the supernova’s light curve, or its luminosity as a function of time. In particular, a Type II supernova can have almost no decrease in brightness as a function of time; it seems to “plateau.” While we’re not entirely sure, we believe that this phenomena is caused by the outer layer of hydrogen being excited (or ionized) by the supernova. The ionized hydrogen basically stops other photons from escaping, thus making it impossible for the luminosity to decrease. Eventually the supernova will cool and the supernova dims as we expect.
The authors of today’s paper are interested in shedding light on what attributes of the star lead to the features we see in these types of supernovae, called Type II-L supernovae (where the “L” stands for “Linear”, as in linear decay).
The Mysterious “Bump”
The authors combine two popular programs to generate fake supernova light curves. First, they generate a progenitor star using the a program called MESAstar. Using this simulation, they’re able to change the amount of mass a star loses over its lifetime to beef-up that star’s outer hydrogen envelope. When their stars are ready to explode, they pass them off to another program known as STELLA. STELLA follows packets of atoms to see how they mix and heat during the supernova explosion. STELLA lets astronomers see these interactions at different frequencies, so they can map the results onto filters we can observe, like the V-band. Figure 2 shows some of the light curves the authors get from STELLA and how they compare with real Type II-L supernovae.
Admittedly, these theoretical models don’t do a perfect job at recreating the observed characteristics of Type II-L supernovae. However, the rough similarities in shape suggest that Type II-L supernovae might come from progenitor stars with large hydrogen envelopes, as predicted. The authors focus on what they consider to be the most jarring dissimilarity between theory and observations: an extra “bump” or re-brightening in the light curves right before the plateau drops off. You can see this in Figure 2 around 30 days for the dark blue model. In more models, this bump is fairly large and noticeable for a large range of parameters, but this bump is not notably pronounced in observed supernovae.
The lack of this bump is itself a clue about the progenitors, because it rules out a lot of possibilities that produce the bump. In particular, the authors point out that larger progenitors would generally be brighter which washes out the bump. Additionally, larger progenitors mean that the hydrogen is less dense; this helps photons to escape more quickly and lead to a fast decline, which is often seen in Type II-L supernovae.
The new hypothesis that larger progenitors might lead to Type II-L supernovae shines light on the importance of catching supernovae early in their explosion. If we catch a supernova before its shock breaks free from the progenitor’s surface, we can definitively measure the progenitor’s size. Unfortunately, the “shock-breakout” happens before we see any other signs of the explosion, so we have to get incredibly lucky to catch such an event!