| Name: | Jeena S K |
| Affiliation: | Indian Institute of Technology Palakkad |
| Conference ID : | ASI2024_247 |
| Title : | Core-Collapse Supernova Origin for LAMOST J1010+2358 |
| Authors : | Jeena S K,
Projjwal Banerjee, and
Alexander Heger
|
| Authors Affiliation: | Department of Physics, Indian Institute of Technology Palakkad, Kerala, India,
School of Physics and Astronomy, Monash University, Vic 3800, Australia |
| Mode of Presentation: | Oral |
| Abstract Category : | Stars, Interstellar Medium, and Astrochemistry in Milky Way |
| Abstract : | Massive stars with an initial mass of $\sim 140$--$260\,\Msun$ with low metallicity are expected to end their lives as pair-instability supernovae (PISNe). They result in a drastically different elemental abundance pattern compared to regular core-collapse supernovae (CCSNe) and are expected to be observed in very metal-poor (VMP) stars. Although many VMP stars have been detected, the unique abundance pattern expected from PISNe has not been unambiguously observed. However, the recently discovered star LAMOST J1010+2358 with metallicity ${\rm[Fe/H]}\lesssim -2.42$ shows a peculiar abundance pattern that is remarkably well fit by a PISN, indicating the potential first discovery of a bonafide star born from gas polluted by a PISN. We explore whether the abundance pattern in this star can also be explained by regular CCSN models. We calculate the detailed nucleosynthesis in a wide range of CCSN models of Population III and Population II stars of metallicity ${\rm[Fe/H]}=-3$ with masses ranging from $12$--$30\,\Msun$. We find that the observed abundance pattern in LAMOST J1010+2358 can be fit equally well by CCSN models of $\sim 12$--$14\,\Msun$ that undergo negligible fallback following the explosion.
We conclude that the measured abundance pattern could have originated from a CCSN and cannot be unambiguously identified with a PISN.
We identify key elements that need to be measured in future detections in stars like LAMOST J1010+2358 that can differentiate between CCSN and PISN origin. |
