Non-accumulation of background-enhanced neutrino forces in proto-neutron stars
Abstract
In a neutrino background, the vacuum two-neutrino exchange potential V ∝ GF2 /r5 acts as a much longer-ranged interaction, scaling as V∼1/r for a directional background. A proto-neutron star (PNS) hosts one of the densest astrophysical neutrino environments known, and naturally provides a setting in which to test whether this pairwise enhancement produces a macroscopic Hartree contribution. We show that this does not happen. In the spin-independent sector, averaging over pair orientations projects the background onto its angular monopole. The bulk Hartree contribution then saturates instead of growing with system size. We also find that the spin-dependent parity-conserving and parity-violating terms do not generate macroscopic growth under the PNS mean-field conditions considered here. Thus, although the pair potential can be strongly enhanced, the resulting bulk interaction remains very small. The suppression comes from the angular and oscillatory structure of the kernel, not from screening. Within the Standard Model mechanism considered here, the effect is not important for the PNS equation of state or for events like pulsar kicks.
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BibTeX
@misc{bora2026nonaccumulation,
title = {{Non-accumulation of background-enhanced neutrino forces in proto-neutron stars}},
author = {Himanshu Bora and Anupam Deka and Debajyoti Dutta},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.17346},
eprint = {2610.17346},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.17346},
note = {CC BY-NC-ND 4.0},
}
RIS
TY - UNPB
TI - Non-accumulation of background-enhanced neutrino forces in proto-neutron stars
AU - Himanshu Bora
AU - Anupam Deka
AU - Debajyoti Dutta
PY - 2026
DA - 2026/10/12
PB - arXiv
DO - 10.48550/arxiv.2610.17346
UR - https://arxiv.org/abs/2610.17346
AB - In a neutrino background, the vacuum two-neutrino exchange potential V ∝ G_F^2 /r^5 acts as a much longer-ranged interaction, scaling as V∼1/r for a directional background. A proto-neutron star (PNS) hosts one of the densest astrophysical neutrino environments known, and naturally provides a setting in which to test whether this pairwise enhancement produces a macroscopic Hartree contribution. We show that this does not happen. In the spin-independent sector, averaging over pair orientations projects the background onto its angular monopole. The bulk Hartree contribution then saturates instead of growing with system size. We also find that the spin-dependent parity-conserving and parity-violating terms do not generate macroscopic growth under the PNS mean-field conditions considered here. Thus, although the pair potential can be strongly enhanced, the resulting bulk interaction remains very small. The suppression comes from the angular and oscillatory structure of the kernel, not from screening. Within the Standard Model mechanism considered here, the effect is not important for the PNS equation of state or for events like pulsar kicks.
ER -