Related Experiment Video
Updated: Oct 2, 2025
06:48
Surface Mapping of Earth-like Exoplanets using Single Point Light Curves
Published on: May 10, 2020
3.7K
Search for Sub-Solar Mass Binaries with Einstein Telescope and Cosmic Explorer
1Divisão de Astrofísica, Instituto Nacional de Pesquisas Espaciais, Avenida dos Astronautas 1758, São José dos Campos 12227-010, SP, Brazil.
Entropy (Basel, Switzerland)
|February 25, 2022
Summary
Detecting sub-solar mass black hole binaries with next-gen gravitational wave detectors like the Einstein Telescope and Cosmic Explorer could reveal exotic objects and primordial black hole abundances.
Area of Science:
- Astrophysics
- Cosmology
- Gravitational Wave Astronomy
Background:
- The detection of sub-solar mass ultra-compact objects could challenge existing black hole formation theories.
- Understanding these objects offers new insights into the universe's fundamental properties.
Purpose of the Study:
- Investigate the significance of detecting sub-solar mass binaries within the sensitivity range of third-generation gravitational wave detectors.
- Explore the implications for primordial black hole abundances.
Main Methods:
- Simulated detection of sub-solar mass binary systems (10^-2 to 1 solar mass) using Einstein Telescope (ET) and Cosmic Explorer (CE) sensitivity.
- Calculated maximum horizon distances for binary detection.
- Derived merger rates and estimated primordial black hole (PBH) abundances.
Main Results:
- ET and CE can detect ultra-compact binaries up to 1.89 Gpc and 5.8 Gpc, respectively.
- The study estimates upper limits on primordial black hole abundance: fPBH < 0.70 for ET and fPBH < 0.06 for CE.
Conclusions:
- Detection of sub-solar mass binaries by ET and CE will significantly constrain primordial black hole formation scenarios.
- This research opens new avenues for understanding exotic compact objects and the early universe.
Related Concept Videos
01:10Detection of Black Holes
2.3K
Although black holes were theoretically postulated in the 1920s, they remained outside the domain of observational astronomy until the 1970s.
Their closest cousins are neutron stars, which are composed almost entirely of neutrons packed against each other, making them extremely dense. A neutron star has the same mass as the Sun but its diameter is only a few kilometers. Therefore, the escape velocity from their surface is close to the speed of light.
Not until the 1960s, when the first neutron...
Their closest cousins are neutron stars, which are composed almost entirely of neutrons packed against each other, making them extremely dense. A neutron star has the same mass as the Sun but its diameter is only a few kilometers. Therefore, the escape velocity from their surface is close to the speed of light.
Not until the 1960s, when the first neutron...
2.3K
01:21Schwarzschild Radius and Event Horizon
2.2K
No object with a finite mass can travel faster than the speed of light in a vacuum. This fact has an interesting consequence in the domain of extremely high gravitational fields.
The minimum speed required to launch a projectile from the surface of an object to which it is gravitationally bound so that it eventually escapes the object’s gravitational field is called the escape velocity. The escape velocity is independent of the mass of the object. Merging the idea of escape...
The minimum speed required to launch a projectile from the surface of an object to which it is gravitationally bound so that it eventually escapes the object’s gravitational field is called the escape velocity. The escape velocity is independent of the mass of the object. Merging the idea of escape...
2.2K
01:12Reduced Mass Coordinates: Isolated Two-body Problem
1.6K
In classical mechanics, the two-body problem is one of the fundamental problems describing the motion of two interacting bodies under gravity or any other central force. When considering the motion of two bodies, one of the most important concepts is the reduced mass coordinates, a quantity that allows the two-body problem to be solved like a single-body problem. In these circumstances, it is assumed that a single body with reduced mass revolves around another body fixed in a position with an...
1.6K
01:29Kepler's Second Law of Planetary Motion
4.5K
In the early 17th century, German astronomer and mathematician Johannes Kepler postulated three laws for the motion of planets in the solar system. His first law states that all planets orbit the Sun in an elliptical orbit, with the Sun at one of the ellipse's foci. Therefore, the distance of a planet from the Sun varies throughout its revolution around the Sun.
While in an elliptical orbit, the total energy of the planet is conserved. Therefore, the planet slows down when it is at apogee and...
While in an elliptical orbit, the total energy of the planet is conserved. Therefore, the planet slows down when it is at apogee and...
4.5K
01:22Atomic Emission Spectroscopy: Instrumentation
675
The instrumentation of atomic emission spectrometry (AES) involves various components, including atomization devices that convert samples into gas-phase atoms and ions. There are two main types of atomization devices: continuous and discrete atomizers. Continuous atomizers, like plasmas and flames, introduce samples in a constant stream, while discrete atomizers inject individual samples using syringes or autosamplers. The most common discrete atomizer is the electrothermal atomizer.
675
01:18Kepler's Third Law of Planetary Motion
3.6K
In the early 17th century, German astronomer and mathematician Johannes Kepler postulated three laws for the motion of planets in the solar system. In 1909, he formulated his first two laws based on the observations of his forebears, Nikolaus Copernicus and Tycho Brahe. However, in 1918, he published his third law of planetary motion, which gives a precise mathematical relationship between a planet's average distance from the Sun and the amount of time it takes to revolve around the Sun. It...
3.6K