White dwarf bounds on charged massive particles
Abstract
White dwarfs (WD) effectively act as high-gain amplifiers for relatively small energy deposits within their volume via their supernova instability. In this paper, we consider the ways a galactic abundance of $$\mathcal{O}$$(1)-charged massive relics (i.e., CHAMPs) could trigger this instability, thereby destroying old WD. The dense central core structure formed inside the WD when heavy CHAMPs sink to its center can trigger a supernova via injection of energy during collapse phases, via direct density-enhanced (pycnonuclear) fusion processes of carbon nuclei dragged into the core by the CHAMPs, or via the formation of a black hole (BH) at the center of the WD. In the latter scenario, Hawking radiation from the BH can ignite the star if the BH forms with a sufficiently small mass; if the BH instead forms at large enough mass, heating of carbon nuclei that accrete onto the BH as it grows in size may be able to achieve the same outcome (with the conservative alternative being simply that the WD is devoured by the BH). The known existence of old WD that have not been destroyed by these mechanisms allows us to improve by many orders of magnitude on the existing CHAMP abundance constraints in the regime of large CHAMP mass, $$m_X ~ 10^{11}–10^{18}$$ GeV. Additionally, in certain regions of parameter space, we speculate that this setup could provide a trigger mechanism for the calcium-rich gap transients: a class of anomalous, subluminous supernova events that occur far outside of a host galaxy.
- Publication Date:
- Research Org.:
- Stanford Univ., CA (United States)
- Sponsoring Org.:
- National Science Foundation (NSF); Heising-Simons Foundation; USDOE Office of Science (SC), High Energy Physics (HEP); Gordon and Betty Moore Foundation; Simons Foundation
- OSTI Identifier:
- 1633710
- Alternate Identifier(s):
- OSTI ID: 1802305
- Grant/Contract Number:
- SC0012012; 100495; PHY-1720397; 2015-037; 2018-0765; GBMF7946; PHY-1818899; PHY-1638509; 378243; 2015-038
- Resource Type:
- Published Article
- Journal Name:
- Physical Review D
- Additional Journal Information:
- Journal Name: Physical Review D Journal Volume: 101 Journal Issue: 11; Journal ID: ISSN 2470-0010
- Publisher:
- American Physical Society
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; Astronomy & Astrophysics; Physics
Citation Formats
Fedderke, Michael A., Graham, Peter W., and Rajendran, Surjeet. White dwarf bounds on charged massive particles. United States: N. p., 2020.
Web. doi:10.1103/PhysRevD.101.115021.
Fedderke, Michael A., Graham, Peter W., & Rajendran, Surjeet. White dwarf bounds on charged massive particles. United States. https://doi.org/10.1103/PhysRevD.101.115021
Fedderke, Michael A., Graham, Peter W., and Rajendran, Surjeet. Wed .
"White dwarf bounds on charged massive particles". United States. https://doi.org/10.1103/PhysRevD.101.115021.
@article{osti_1633710,
title = {White dwarf bounds on charged massive particles},
author = {Fedderke, Michael A. and Graham, Peter W. and Rajendran, Surjeet},
abstractNote = {White dwarfs (WD) effectively act as high-gain amplifiers for relatively small energy deposits within their volume via their supernova instability. In this paper, we consider the ways a galactic abundance of $\mathcal{O}$(1)-charged massive relics (i.e., CHAMPs) could trigger this instability, thereby destroying old WD. The dense central core structure formed inside the WD when heavy CHAMPs sink to its center can trigger a supernova via injection of energy during collapse phases, via direct density-enhanced (pycnonuclear) fusion processes of carbon nuclei dragged into the core by the CHAMPs, or via the formation of a black hole (BH) at the center of the WD. In the latter scenario, Hawking radiation from the BH can ignite the star if the BH forms with a sufficiently small mass; if the BH instead forms at large enough mass, heating of carbon nuclei that accrete onto the BH as it grows in size may be able to achieve the same outcome (with the conservative alternative being simply that the WD is devoured by the BH). The known existence of old WD that have not been destroyed by these mechanisms allows us to improve by many orders of magnitude on the existing CHAMP abundance constraints in the regime of large CHAMP mass, $m_X ~ 10^{11}–10^{18}$ GeV. Additionally, in certain regions of parameter space, we speculate that this setup could provide a trigger mechanism for the calcium-rich gap transients: a class of anomalous, subluminous supernova events that occur far outside of a host galaxy.},
doi = {10.1103/PhysRevD.101.115021},
journal = {Physical Review D},
number = 11,
volume = 101,
place = {United States},
year = {Wed Jun 17 00:00:00 EDT 2020},
month = {Wed Jun 17 00:00:00 EDT 2020}
}
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