Manuel Pichardo Marcano (Fisk/Vanderbilt)

Karan Jani

Detection of the most massive white dwarf mergers with LILA

Type Ia Supernova

• Type Ia:
  • I: No H or He
  • a:  strong SiII
• Explosion  of C/O WD
• Chandrasekhar Mass (Mch = 1.4M⊙)
• Cosmological standard candles
  • Hubble Tension
• Output to Galaxies
•  Heavy-element factories

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

• Single Degenerate (WD + Non-degenerate):
  • Symbiotics: WD + RG
  • Novae: WD + MS
  • Supersoft X-ray sources
  • WD + Hot subdwarfs
• Double Degenerate (WD + WD):
  • GW-driven
  • Third-Body-Induced Collisions

Progenitor Problem

Caltech/NASA

No Consensus on Main Mechanism:

EM + GW can solve this problem

• A lot of Open Questions!
• Accretion-induced collapse (AIC)?
  • Formation of Neutron Star
• Detonation mechanism?
• A range of Masses:
  • sub-Mch, Mch, super-Mch
• A range of Luminisities:
  • sub-, normal, super- luminous

Double Degenerates

Gravitational Waves Sources

A multi-messenger approach promises to help solve these problems

LISA and LILA

• LISA:
  • Millihertz
  • SNe Ia progenitors in the Milky way
• LILA:
  • More sensitive to higher masses at greater distances (> 0.1 Hz)
  • Probe the merger in other galaxies

Methods

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

LISA

GLOC

LISA vs GLOC

LISA vs GLOC

Best Case Scenario

SNR = 15 at 10 Mpc

Best Case Scenario

SNR = 15 at 10 Mpc

1.4 + 1.4 M⊙

LILA

• LILA will help a lot:
  • 0.1 Hz vs 0.25 Hz (GLOC)

Future Work for the Paper

• Expected SN Rates
• What Masses and combinations of WDs can we expect?
  • ONe + CO WD?
  • CO + CO WD?
• What would a none detection from LILA mean?