Manuel Pichardo Marcano (Fisk/Vanderbilt)

Karan Jani (Vanderbilt)

Detection of the most massive white dwarf mergers with LILA

 

Double WD Binaries

Caltech/NASA

  • Gravitational Wave Sources
  • WDs  with masses 1.3 to 1.4 M⊙
  • Detached
  • Circular Orbit
  • Porb
    • 15 seconds to merge
  • fgrav = 2 x forb

Type Ia Supernova

  • Type Ia
  • Chandrasekhar Mass (Mch = 1.4M⊙)
  • Cosmological standard candles
    • Hubble Tension
  •  Heavy-element factories

R. Sankrit and W. Blair (JHU) et al., ESA, NASA

Accretion-induced Collapse

  • Formation of Neutron Stars (e.g. Nomoto et al. 1979)
  • Important in GCs (Grindlay et al. 1988)
  • Predicted EM:
    • Gamma Rays (e.g. Dar et al. 1992)
    • Radio (e.g. Piro et al. 2013)
    • Optical (Sousa et al. 2023)

NASA, ESA, and J. Anderson (STScI)

Lunar Gravitational Wave Observatories

  • The Lunar Gravitational-wave Antenna (LGWA) (Parameswaran et al. 2024)
    • Seismometer
  • Laser Interferometer Lunar Antenna (LILA):
    • LIGO-like suspension system

Methods

  • Evolve WDs  with masses 1.3 to 1.4 M⊙
  • 4 years before merging:
    • Roche-lobe: Lower Mass Fills Roche Lobe
    • Contact: a = R1+R2
  • Calculate SNR for LGWA and Gravitational-Wave Lunar Observatory for Cosmology (GLOC) as a LILA proxy

 

Wagg et al. (2022)
Dupletsa et al. (2023)

Strain

Horizon Distance

Horizon Distance

Early Alert at 10 Mpc

Early Alert at 10 Mpc

GWs from the Moon

  • GW freq. between LISA and LIGO
  • Massive WDs merger at Mpc distances
    • Weeks of Early Alert
    • Multi-Messenger Astrophysics
  • WDs + NS
  • WDs + Primordial BHs