MIT Libraries logoDSpace@MIT

MIT
View Item 
  • DSpace@MIT Home
  • MIT Open Access Articles
  • MIT Open Access Articles
  • View Item
  • DSpace@MIT Home
  • MIT Open Access Articles
  • MIT Open Access Articles
  • View Item
JavaScript is disabled for your browser. Some features of this site may not work without it.

Exploring the formation mechanisms of double neutron star systems: an analytical perspective

Author(s)
Taani, Ali; Abu-Saleem, Mohammed; Mardini, Mohammad; Aljboor, Hussam; Tayem, Mohammad
Download10509_2025_4433_ReferencePDF.pdf (Embargoed until: 2026-05-08, 1.056Mb)
Publisher Policy

Publisher Policy

Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.

Terms of use
Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.
Metadata
Show full item record
Abstract
Double Neutron Stars (DNSs) are unique probes to study various aspects of modern astrophysics. Recent discoveries have confirmed direct connections between DNSs and supernova explosions. This provides valuable information about the evolutionary history of these systems, especially regarding whether the second-born Neutron Star (NS) originated from either a Core-Collapse ( C C ) or Electron-Capture Supernovae ( E C S N e ) event. The provided scale diagram illustrates the distribution of different types of DNSs on the basis of their orbital parameters and other factors, including mass loss. As a result, the physical processes in DNSs vary depending on the formation mechanisms of the second-born NS and characteristics of the systems. E C S N e processes are typically associated with merging systems ( e × P o r b < 0.05 ), while C C processes are more commonly linked to non-merging systems ( e × P o r b > 0.05 ). Our results suggest a critical mass threshold of 1.30 M ⊙ ± 0.22 M ⊙ (critical value) for the E C S N e process to form an NS, while C C processes might occur at higher masses. Examining the orbital parameters of DNSs in a known gravitational potential can enhance our understanding of the theoretical predictions for DNS progenitor characteristics. It turns out that the E C S N e process predominantly produces DNS systems with short orbital ( P o r b ≤ 0.25 d ), nearly circular orbits ( e ≃ 0.2 ), accompanied by minimal kick velocities imparted on the proto-NS and significant mass loss. In contrast, their orbital dynamics in a known gravitational potential plays a crucial role in enhancing our understanding of the SNe geometry and the formation and evolution processes among different NS samples.
Date issued
2025-05-08
URI
https://hdl.handle.net/1721.1/159261
Department
Massachusetts Institute of Technology. Department of Physics; MIT Kavli Institute for Astrophysics and Space Research
Journal
Astrophysics and Space Science
Publisher
Springer Netherlands
Citation
Taani, A., Abu-Saleem, M., Mardini, M. et al. Exploring the formation mechanisms of double neutron star systems: an analytical perspective. Astrophys Space Sci 370, 42 (2025).
Version: Author's final manuscript

Collections
  • MIT Open Access Articles

Browse

All of DSpaceCommunities & CollectionsBy Issue DateAuthorsTitlesSubjectsThis CollectionBy Issue DateAuthorsTitlesSubjects

My Account

Login

Statistics

OA StatisticsStatistics by CountryStatistics by Department
MIT Libraries
PrivacyPermissionsAccessibilityContact us
MIT
Content created by the MIT Libraries, CC BY-NC unless otherwise noted. Notify us about copyright concerns.