The Gradual Disruption of Stars by Black Holes
Learn about tidal peeling events and their impact on stars near black holes.
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Table of Contents
Close encounters between black holes and stars happen often in areas with many stars, such as star clusters and the centers of galaxies. When a black hole gets too close to a star, it can pull the star apart, causing the star to lose mass in a dramatic event. This is called a Tidal Disruption Event (TDE). The outcome can lead to bursts of light that we can observe from Earth.
Most of the time, these encounters happen quickly, and the star is pulled apart in a flash. However, there is another possibility: the star can approach the black hole slowly, almost in a circle, losing its mass over time rather than all at once. This slow process is known as a tidal peeling event (TPE).
What Happens in a Tidal Peeling Event?
In a TPE, a star moves close to a black hole and begins to lose its outer layers. This happens gradually over many orbits instead of one sudden event. During the process, the black hole continues to pull on the star, stripping away layers and causing the star to change shape. Over time, some of the star's material gets pulled into the black hole, while other parts may get flung away into space.
The way a star is affected during a TPE can be visualized as peeling layers off an onion. The outer layers are removed slowly, allowing the star to keep its shape longer than if it was completely disrupted all at once.
Conditions for a Tidal Peeling Event
For a TPE to occur, certain conditions have to be met:
Star's Orbit: The star must have a nearly circular path around the black hole, known as low eccentricity. This means the star isn't swinging in and out quickly, but rather moving steadily around the black hole.
Distance from the Black Hole: The star needs to start at a distance that allows it to be pulled in by the black hole's gravity without being completely torn apart right away.
Mass of the Star: The size and mass of the star also play a role. More massive stars can lose mass more quickly because they are larger and have more material for the black hole to grab onto.
Observations and Simulations
To better understand TPEs, scientists have used computer simulations to model how stars behave when they come close to black holes. In these simulations, they create scenarios with different star sizes, initial distances, and paths to visualize the peeling process.
From these studies, we learn that TPEs are quite different from the fast and bright disruptions of typical TDEs. A star in a TPE can last multiple orbits around a black hole while losing material gradually. This slow loss can affect how bright the event appears to us from Earth.
Light and Energy from Tidal Peeling Events
When a star loses material to a black hole, that falling material can become heated and emit light. In a TPE, because the process is more gradual, the light emitted can behave differently compared to the bright flash of a single disruption event. The energy released can sometimes be more subdued and may take a longer time to peak.
This difference in how light is emitted means that TPEs might not be detected as readily as other events. They can get lost among the other emissions from the black hole and surrounding area. However, scientists are continuing to refine their models and observational techniques to identify these events.
Importance of Tidal Peeling Events
Understanding TPEs helps scientists learn more about the conditions around black holes and how they interact with the stars they encounter. They provide insights into the dynamics of star clusters and the behavior of very dense environments in space.
Moreover, TPEs offer a new way to think about how mass transfer happens between stars and black holes. Identifying and studying these events can eventually improve our ability to observe and understand many cosmic processes, such as star formation and black hole growth.
Future Studies
Going forward, researchers plan to improve their simulations to include even more detailed physical processes, such as how gas behaves and how energy transfers occur during these events. They also want to explore how TPEs might be detected among various cosmic phenomena.
As telescopes and observational techniques improve, the chances of spotting TPEs and understanding their signatures will increase. This can help scientists gain more knowledge about the fundamental interactions between stars and black holes, and the role these events play in the broader universe.
Conclusion
Tidal peeling events give us a new perspective on the relationship between black holes and stars. By examining these slow, gradual interactions, scientists can uncover more about the complexities of the cosmos and the beautiful intricacies involved in stellar dynamics. The continued study of TPEs not only deepens our knowledge of black holes but also enhances our understanding of the universe's evolution.
Title: Tidal Peeling Events: low-eccentricity tidal disruption of a star by a stellar-mass black hole
Abstract: Close encounters between stellar-mass black holes (BHs) and stars occur frequently in dense star clusters and in the disks of active galactic nuclei (AGNs). Recent studies have shown that in highly eccentric close encounters, the star can be tidally disrupted by the BH (micro-tidal disruption event, or micro-TDE), resulting in rapid mass accretion and possibly bright electromagnetic signatures. Here we consider a scenario in which the star might approach the stellar-mass BH in a gradual, nearly circular inspiral, under the influence of dynamical friction on a circum-binary gas disk or three-body interactions in a star cluster. We perform hydro-dynamical simulations of this scenario using the smoothed particle hydrodynamics code PHANTOM. We find that the mass of the star is slowly stripped away by the BH. We call this gradual tidal disruption a "tidal-peeling event", or a TPE. Depending on the initial distance and eccentricity of the encounter, TPEs might exhibit significant accretion rates and orbital evolution distinct from those of a typical (eccentric) micro-TDE.
Authors: Chengcheng Xin, Zoltan Haiman, Rosalba Perna, Yihan Wang, Taeho Ryu
Last Update: 2023-03-22 00:00:00
Language: English
Source URL: https://arxiv.org/abs/2303.12846
Source PDF: https://arxiv.org/pdf/2303.12846
Licence: https://creativecommons.org/licenses/by/4.0/
Changes: This summary was created with assistance from AI and may have inaccuracies. For accurate information, please refer to the original source documents linked here.
Thank you to arxiv for use of its open access interoperability.