LISA detecting gravitational waves from a double white dwarf in Andromeda

Hunting Gravitational Waves: LISA's Quest to Uncover Hidden Worlds in Neighboring Galaxies

Avery Sinclair in Science & Nature August 2025 • 4 min read.

"Explore how LISA, the Laser Interferometer Space Antenna, could revolutionize our understanding of double white dwarf binaries and their role in mapping the Local Group of galaxies."

The Laser Interferometer Space Antenna (LISA) is set to revolutionize our understanding of the universe by detecting gravitational waves from various cosmic sources. Among these, detached double white dwarf (DWD) binaries stand out as primary targets. These systems, consisting of two white dwarf stars orbiting each other, are not only abundant but also serve as crucial tools for probing binary evolution, understanding the formation channels of Type Ia supernovae (SNIa), and mapping the structure of our galaxy, the Milky Way.

Until now, predictions about the detectability of DWDs have largely focused on the Milky Way. However, a recent study sheds light on LISA's potential to detect these binaries in neighboring galaxies within the Local Group, including the Large and Small Magellanic Clouds (LMC and SMC), and even as far as Andromeda (M31). This breakthrough opens up exciting possibilities for studying stellar populations beyond our galactic borders.

This article delves into how LISA can identify DWDs in these distant galaxies, focusing on the shortest orbital periods and highest total masses, pinpointing potential double-degenerate SNIa progenitors. These binaries are particularly challenging to detect using traditional optical telescopes, making LISA an invaluable asset for determining SNIa merger rates across the Local Group.

Unlocking the Secrets of Gravitational Waves: How LISA Will Detect Double White Dwarfs?

LISA detecting gravitational waves from a double white dwarf in Andromeda

LISA's ability to detect gravitational waves hinges on several key factors, primarily the characteristics of the DWD binaries themselves, such as their orbital periods and chirp masses. The chirp mass is a measure of the mass of the binary system that can be detected and is calculated as the mass of both objects in the system. The distance to these binaries also plays a critical role. The strength of the gravitational wave signal diminishes with distance, making closer binaries easier to detect.

To estimate LISA's detection capabilities, researchers consider the signal-to-noise ratio (S/N). A higher S/N indicates a stronger, more easily detectable signal. The S/N depends on the amplitude of the gravitational wave, the instrument's sensitivity, and the duration of the observation. By analyzing these factors, scientists can predict which DWDs are most likely to be detected by LISA.

Orbital Period: LISA is particularly sensitive to DWDs with short orbital periods (less than 1 hour).
Chirp Mass: Binaries with higher chirp masses produce stronger gravitational wave signals.
Distance: DWDs in the Local Group, such as those in the LMC, SMC, and M31, are within LISA's detection range.
Mission Duration: Longer observation times increase the likelihood of detecting weaker signals.

Researchers have created detailed models to simulate DWD populations in these galaxies. These models, combined with LISA's expected performance, allow scientists to estimate the number of DWDs that LISA will detect. For example, simulations suggest that LISA could detect dozens of DWDs in M31 within a few years of operation.

The Future of Gravitational Wave Astronomy: Detecting the Undetectable

LISA's mission extends beyond simply detecting DWDs. By precisely measuring the properties of these binaries, LISA will provide unprecedented insights into stellar evolution, binary formation, and the structure of galaxies within the Local Group. Moreover, LISA's ability to detect DWDs that are too faint for optical telescopes opens a new window into studying potential SNIa progenitors, helping us better understand the origins of these powerful cosmic explosions. With LISA, the universe is set to reveal its hidden gravitational secrets, transforming our understanding of the cosmos.

About this Article -

This article was crafted using a human-AI hybrid and collaborative approach. AI assisted our team with initial drafting, research insights, identifying key questions, and image generation. Our human editors guided topic selection, defined the angle, structured the content, ensured factual accuracy and relevance, refined the tone, and conducted thorough editing to deliver helpful, high-quality information.See our About page for more information.

This article is based on research published under:

DOI-LINK: 10.3847/2041-8213/aae587, Alternate LINK

Title: Detectability Of Double White Dwarfs In The Local Group With Lisa

Subject: Space and Planetary Science

Journal: The Astrophysical Journal

Publisher: American Astronomical Society

Authors: Valeria Korol, Orlin Koop, Elena M. Rossi

Published: 2018-10-15

Everything You Need To Know

What is LISA, and how will it contribute to our understanding of double white dwarf binaries?

LISA, or the Laser Interferometer Space Antenna, is designed to detect gravitational waves from cosmic sources, including detached double white dwarf (DWD) binaries. These systems, consisting of two white dwarf stars orbiting each other, are valuable for studying binary evolution, understanding the formation of Type Ia supernovae (SNIa), and mapping the structure of galaxies like the Milky Way. LISA will measure the gravitational waves emitted by these binaries, providing insights that are difficult to obtain through traditional methods.

What factors influence LISA's ability to detect double white dwarf binaries, and how do scientists estimate its detection capabilities?

LISA's ability to detect double white dwarf (DWD) binaries depends on several factors. These include the orbital periods of the binaries (with LISA being particularly sensitive to those with short orbital periods), their chirp masses (where higher chirp masses produce stronger signals), and their distance from LISA (with closer binaries being easier to detect). The mission duration also matters, as longer observation times increase the likelihood of detecting weaker signals. By considering these factors, scientists can predict which DWDs are most likely to be detected.

How will LISA contribute to our understanding of Type Ia supernovae progenitors, and why is this important for cosmology?

LISA's mission will help scientists understand the potential double-degenerate Type Ia supernovae (SNIa) progenitors. By detecting double white dwarf (DWD) binaries that are too faint for optical telescopes, LISA opens a new avenue for studying the origins of these cosmic explosions. This is crucial because understanding SNIa is essential for measuring cosmic distances and understanding the expansion of the universe. LISA will help refine the models used to predict SNIa merger rates across the Local Group.

Beyond the Milky Way, where else might LISA detect double white dwarf binaries, and why is this significant for studying stellar populations?

LISA has the potential to detect double white dwarf (DWD) binaries in neighboring galaxies within the Local Group, including the Large and Small Magellanic Clouds (LMC and SMC), and even Andromeda (M31). This is significant because it allows us to study stellar populations beyond our galaxy. By detecting DWDs in these galaxies, LISA can provide insights into stellar evolution and the structure of the Local Group, expanding our understanding of the universe beyond the Milky Way.

How do researchers use models and simulations to estimate the number of double white dwarf binaries LISA will detect in other galaxies?

Researchers use detailed models and simulations of double white dwarf (DWD) populations in galaxies to estimate LISA's detection capabilities. These models, combined with LISA's expected performance, allow scientists to predict the number of DWDs that LISA might detect. For instance, simulations suggest that LISA could detect dozens of DWDs in Andromeda (M31) within a few years of operation. These predictions are essential for planning observations and maximizing the scientific return from LISA's mission.