GW-EOS Working Group (first period)

Gravitational Wave and Equation of State Working Group (first period) (February 1st 2020 - January 31st 2024)

Objectives

The Laser Interferometer GW Observatory (LIGO) and Virgo have operated the third observing run (O3 run) until March 2020. In addition, the Japanese detector, KAGRA, has finally entered the detector network since 2020. Furthermore, discussion for the third-generation GW detectors, such as the Einstein Telescope and Cosmic Explorer, has already been started. With these detectors, it is expected that the number of GW events would increase more and more in the near future. In such an era, the GWs from not only the compact binary mergers but also core-collapse supernova explosions might be detected.

Due to quite the high permeability of GWs, one expects to get raw information of source objects via GW observations. This is one of the significances for detecting the GWs. That is, through the GW observations, one may see “invisible” interior properties. In this working group, we especially focus on the following points:

  1. Understanding the GW spectrum from the core-collapse supernova
  2. Finding the universal relation in GW frequencies
  3. Discussion and exploration of the newly obtained GW data
Facilitators:
Hajime Sotani (RIKEN) *Contact at hajime.sotani@riken.jp
Tomoya Takiwaki (NAOJ)
Hajime Togashi (Tohoku University)

Akira Dohi (Kyushu University)

Former Objectives (2020)

Since April 2019, the Laser Interferometer GW Observatory (LIGO) and Virgo have been operating as third observing run (O3 run) until April 2020. In addition to these GW detectors, the Japanese detector, KAGRA, has also started the engineering run since December 2019, and will start an observation run after February 2020. Furthermore, discussion for the third-generation GW detectors, such as the Einstein Telescope and Cosmic Explorer, has already been started. With these detectors, it is expected that the number of GW events would increase more and more in the near future. In such an era, the GWs from not only the compact binary mergers but also core-collapse supernova explosions might be detected.

Due to quite high permeability of GWs, one expects to get raw information of source objects via GW observations. This is one of the significances for detecting the GWs. That is, through the GW observations, one may see “invisible” interior properties. In this working group, we especially focus on the following points:

  1. Understanding the GW spectrum from the core-collapse supernova
  2. Finding the universal relation in GW frequencies
  3. Associating the GW frequencies with the nuclear saturation parameters
  4. Discussion and exploration of the newly obtained GW data