First author institution: Caltech
Status: published in ApJ, open access version available
Massive stars die as core collapse supernovae: the star can no longer produce the nuclear reactions that balance its strong gravity, and the star collapses onto its core. When this happens, large amounts of energy and neutrons are available to form elements heavier than iron. The distribution of elements produced in the deepest layers of the star as it goes supernova is key to understanding the mechanism by which the collapse of the star leads to an explosion.Radioactive decay powers the optical light emitted by the supernova ~ 50−100 days after the explosion. In fact, we can still see radioactive signatures in remnants that are hundreds of years old. In today’s paper, the authors use high energy X-ray satellite NuStar observations to study the distribution of 44Ti in the young supernova remnant Cassiopeia A (Cas A). The current distribution of radioactive elements and their decay products is linked to the local conditions in which they were synthesised when the explosion took place. Therefore, knowing where the 44Ti is now can shed light on the details of the supernova event that ended the life of Cas A’s progenitor star.
The Cas A Supernova Remnant
Cas A is known by radio astronomers as one of the brightest radio sources in the sky, although the bulk of its energy is emitted as thermal X-rays. These are produced as the ejecta from the star encounter the supernova remnant shock, and it heats them to X-ray emitting temperatures. Shocks are transition layers in which the thermodynamic properties of a plasma change rapidly, and that arise whenever some material moves faster than the local speed of sound. Supernova remnants can show two kinds of shocks: the forward shock, which is the blast wave from the supernova explosion, and a reverse shock that forms as the forward shock bounces back when it encounters dense circumstellar material. We think Cas A’s explosion date is 1672, although there are no definite records of it being observed. It is one of the few historical supernova remnants found to be of type IIb from its light echoes (read this Astrobite for the details of supernova classification and this Astrobite to find out what makes light echoes such a mind blowing astronomical technique).
Radioactive elements and the explosion
The production of radioactive elements is very sensitive to local conditions of density and temperature during explosive nucleosynthesis and can give us clues on the nature of the explosion mechanism. 44Ti has a half life of ~ 58 years, which means there is still a small amount of 44Ti in Cas A decaying. We can see these decays as high energy lines within the frequency range of NuStar. In fact, the mass of 44Ti we measure today is directly proportional to its original mass, independent of what has happened to the ejecta in the 340 years since explosion. Another important radioactive product of explosive nucleosynthesis is 56Ni. Unlike 44Ti , 56Ni has a short half-life, ∼ 6 days, which means we can only know its original abundance from the abundance of its stable decay product 56Fe.
The authors use the NuStar satellite to map 44Ti with 18” resolution (see Figure 1; the size of Cas A is 5’). Their aim is to get a velocity for each 44Ti clump. The velocity vector has two components in the plane of the sky, which they can get from interpolating the current position of a clump to the center of expansion (which for Cas A has been measured quite reliably) and assuming that the ejecta expand freely. The third component of the velocity vector, the line of sight component, can be measured from the red and blue doppler shifting of the lines coming from each spatially resolved clump—recall that an X-ray telescope labels the energy of each incoming photon.
The authors find that almost all of the 44Ti is moving in the opposite direction of Cas A’s central compact object (CCO). The CCO is a neutron star that we think is the compact remnant of the supernova explosion. It is off-centre, so we believe that it received a ‘kick’ at the time of the explosion. Since the 44Ti is moving in the opposite direction, it can be part of the material that gave the neutron star its kick (from momentum conservation). They also find that there are regions where they see 44Ti and Fe, regions with 44Ti and no Fe, and regions with Fe and no 44Ti (recall that Fe is the decay product of 56Ni). Since the ratio of 56Ni to 44Ti is sensitive to the local conditions during the explosion, these observations suggest that the local conditions of the supernova shock during explosive nucleosynthesis were varied, and so there were large scale asymmetries in densities of the innermost ejecta when the star went supernova.
Perhaps it is not so surprising that core-collapse supernovae are complicated events. In the case of Cas A, 4-6 solar masses of material collapsed on itself, part of it forming a neutron star, and part of it was somehow expelled outward and is now interacting with the medium around it. The asymmetries evident from element distributions result in a shell that is surprisingly spherical. There are clearly many details left to iron out as to how all of this happens. Works such as this one can offer us a (radioactive) glimpse into how it all fits together.
neat stuff here!