Comparison of the Core-Collapse Evolution of Two Nearly Equal Mass Progenitors
| Title: | Comparison of the Core-Collapse Evolution of Two Nearly Equal Mass Progenitors |
|---|---|
| Authors: | Bruenn, Stephen W., Sieverding, Andre, Lentz, Eric J., Sukhbold, Tuguldur, Hix, W. Raphael, Huk, Leah N., Harris, J. Austin, Messer, O. E. Bronson, Mezzacappa, Anthony |
| Source: | ApJ, 2023, 497, 35 |
| Publication Year: | 2022 |
| Collection: | Astrophysics |
| Subject Terms: | Astrophysics - Solar and Stellar Astrophysics |
| More Details: | We compare the core-collapse evolution of a pair of 15.8 $M_\odot$ stars with significantly different internal structures, a consequence of bimodal variability exhibited by massive stars during their late evolutionary stages. The 15.78 and 15.79 $M_\odot $ progenitors have core masses of 1.47 and 1.78 $M_\odot$ and compactness parameters $\xi_{1.75}$ of 0.302 and 0.604. The core collapse simulations are carried out in 2D to nearly 3 s post-bounce and show substantial differences in the times of shock revival and explosion energies. The 15.78 $M_\odot$ model explodes promptly at 120 ms post-bounce when a strong density decrement at the Si--Si/O shell interface encounters the stalled shock. The 15.79 $M_\odot$ model, which lacks the density decrement, takes 100 ms longer to explode but ultimately produces a more powerful explosion. Larger mass accretion rate of the 15.79 $M_\odot$ model during the first 0.8 s post-bounce results in larger $\nu_{e}$/$\bar \nu_{e}$ luminosities and rms energies. The $\nu_{e}$/$\bar \nu_{e}$ luminosities and rms energies arising from the inner core are also larger in the 15.79 $M_\odot$ model throughout due to the larger negative temperature gradient of this core due to greater adiabatic compression. Larger luminosities and rms energies in the 15.79 $M_\odot$ model and a flatter and higher density heating region, result in more energy deposition behind the shock and more ejected matter with higher enthalpy. We find the ejected $^{56}$Ni mass of the 15.79 $M_\odot$ model is more than double that of the 15.78 $M_\odot$ model. Most of the ejecta in both models is moderately proton-rich, though counterintuitively the highest electron fraction ($Y_e=0.61$) ejecta in either model is in the less energetic 15.78 $M_\odot$ model while the lowest electron fraction ($Y_e=0.45$) ejecta in either model is in the 15.79 $M_\odot$ model. Comment: 24 pages; Accepted for publication in ApJ |
| Document Type: | Working Paper |
| DOI: | 10.3847/1538-4357/acbb65 |
| Access URL: | http://arxiv.org/abs/2211.12675 |
| Accession Number: | edsarx.2211.12675 |
| Database: | arXiv |
| FullText | Text: Availability: 0 CustomLinks: – Url: http://arxiv.org/abs/2211.12675 Name: EDS - Arxiv Category: fullText Text: View this record from Arxiv MouseOverText: View this record from Arxiv – Url: https://resolver.ebsco.com/c/xy5jbn/result?sid=EBSCO:edsarx&genre=article&issn=&ISBN=&volume=&issue=&date=20221122&spage=&pages=&title=Comparison of the Core-Collapse Evolution of Two Nearly Equal Mass Progenitors&atitle=Comparison%20of%20the%20Core-Collapse%20Evolution%20of%20Two%20Nearly%20Equal%20Mass%20Progenitors&aulast=Bruenn%2C%20Stephen%20W.&id=DOI:10.3847/1538-4357/acbb65 Name: Full Text Finder (for New FTF UI) (s8985755) Category: fullText Text: Find It @ SCU Libraries MouseOverText: Find It @ SCU Libraries |
|---|---|
| Header | DbId: edsarx DbLabel: arXiv An: edsarx.2211.12675 RelevancyScore: 1043 AccessLevel: 3 PubType: Report PubTypeId: report PreciseRelevancyScore: 1043.48291015625 |
| IllustrationInfo | |
| Items | – Name: Title Label: Title Group: Ti Data: Comparison of the Core-Collapse Evolution of Two Nearly Equal Mass Progenitors – Name: Author Label: Authors Group: Au Data: <searchLink fieldCode="AR" term="%22Bruenn%2C+Stephen+W%2E%22">Bruenn, Stephen W.</searchLink><br /><searchLink fieldCode="AR" term="%22Sieverding%2C+Andre%22">Sieverding, Andre</searchLink><br /><searchLink fieldCode="AR" term="%22Lentz%2C+Eric+J%2E%22">Lentz, Eric J.</searchLink><br /><searchLink fieldCode="AR" term="%22Sukhbold%2C+Tuguldur%22">Sukhbold, Tuguldur</searchLink><br /><searchLink fieldCode="AR" term="%22Hix%2C+W%2E+Raphael%22">Hix, W. Raphael</searchLink><br /><searchLink fieldCode="AR" term="%22Huk%2C+Leah+N%2E%22">Huk, Leah N.</searchLink><br /><searchLink fieldCode="AR" term="%22Harris%2C+J%2E+Austin%22">Harris, J. Austin</searchLink><br /><searchLink fieldCode="AR" term="%22Messer%2C+O%2E+E%2E+Bronson%22">Messer, O. E. Bronson</searchLink><br /><searchLink fieldCode="AR" term="%22Mezzacappa%2C+Anthony%22">Mezzacappa, Anthony</searchLink> – Name: TitleSource Label: Source Group: Src Data: ApJ, 2023, 497, 35 – Name: DatePubCY Label: Publication Year Group: Date Data: 2022 – Name: Subset Label: Collection Group: HoldingsInfo Data: Astrophysics – Name: Subject Label: Subject Terms Group: Su Data: <searchLink fieldCode="DE" term="%22Astrophysics+-+Solar+and+Stellar+Astrophysics%22">Astrophysics - Solar and Stellar Astrophysics</searchLink> – Name: Abstract Label: Description Group: Ab Data: We compare the core-collapse evolution of a pair of 15.8 $M_\odot$ stars with significantly different internal structures, a consequence of bimodal variability exhibited by massive stars during their late evolutionary stages. The 15.78 and 15.79 $M_\odot $ progenitors have core masses of 1.47 and 1.78 $M_\odot$ and compactness parameters $\xi_{1.75}$ of 0.302 and 0.604. The core collapse simulations are carried out in 2D to nearly 3 s post-bounce and show substantial differences in the times of shock revival and explosion energies. The 15.78 $M_\odot$ model explodes promptly at 120 ms post-bounce when a strong density decrement at the Si--Si/O shell interface encounters the stalled shock. The 15.79 $M_\odot$ model, which lacks the density decrement, takes 100 ms longer to explode but ultimately produces a more powerful explosion. Larger mass accretion rate of the 15.79 $M_\odot$ model during the first 0.8 s post-bounce results in larger $\nu_{e}$/$\bar \nu_{e}$ luminosities and rms energies. The $\nu_{e}$/$\bar \nu_{e}$ luminosities and rms energies arising from the inner core are also larger in the 15.79 $M_\odot$ model throughout due to the larger negative temperature gradient of this core due to greater adiabatic compression. Larger luminosities and rms energies in the 15.79 $M_\odot$ model and a flatter and higher density heating region, result in more energy deposition behind the shock and more ejected matter with higher enthalpy. We find the ejected $^{56}$Ni mass of the 15.79 $M_\odot$ model is more than double that of the 15.78 $M_\odot$ model. Most of the ejecta in both models is moderately proton-rich, though counterintuitively the highest electron fraction ($Y_e=0.61$) ejecta in either model is in the less energetic 15.78 $M_\odot$ model while the lowest electron fraction ($Y_e=0.45$) ejecta in either model is in the 15.79 $M_\odot$ model.<br />Comment: 24 pages; Accepted for publication in ApJ – Name: TypeDocument Label: Document Type Group: TypDoc Data: Working Paper – Name: DOI Label: DOI Group: ID Data: 10.3847/1538-4357/acbb65 – Name: URL Label: Access URL Group: URL Data: <link linkTarget="URL" linkTerm="http://arxiv.org/abs/2211.12675" linkWindow="_blank">http://arxiv.org/abs/2211.12675</link> – Name: AN Label: Accession Number Group: ID Data: edsarx.2211.12675 |
| PLink | https://login.libproxy.scu.edu/login?url=https://search.ebscohost.com/login.aspx?direct=true&site=eds-live&scope=site&db=edsarx&AN=edsarx.2211.12675 |
| RecordInfo | BibRecord: BibEntity: Identifiers: – Type: doi Value: 10.3847/1538-4357/acbb65 Subjects: – SubjectFull: Astrophysics - Solar and Stellar Astrophysics Type: general Titles: – TitleFull: Comparison of the Core-Collapse Evolution of Two Nearly Equal Mass Progenitors Type: main BibRelationships: HasContributorRelationships: – PersonEntity: Name: NameFull: Bruenn, Stephen W. – PersonEntity: Name: NameFull: Sieverding, Andre – PersonEntity: Name: NameFull: Lentz, Eric J. – PersonEntity: Name: NameFull: Sukhbold, Tuguldur – PersonEntity: Name: NameFull: Hix, W. Raphael – PersonEntity: Name: NameFull: Huk, Leah N. – PersonEntity: Name: NameFull: Harris, J. Austin – PersonEntity: Name: NameFull: Messer, O. E. Bronson – PersonEntity: Name: NameFull: Mezzacappa, Anthony IsPartOfRelationships: – BibEntity: Dates: – D: 22 M: 11 Type: published Y: 2022 |
| ResultId | 1 |