Rest-men density (top panel) and angular velocity (bottom panel) on the equatorial plane for a non-magnetized (left column) and magnetized (right column) analog, 10 ms after the merger. White and black lines indicate density figure. There are two main differences between magnetized and nonmagnetized cases 1) In a certain time the magnetized residue is more axial than the more axial (more circular equatorial figure), more axial (more spherical equatorial figure), and 2) the angular velocity in the original of the residue, which is more similar in the remaining case. Credit: Tsocaros et al.
The neutron star merger is a conflict between the neutron stars, which were once a large -scale supergent stars collapsed. These mergers are known to spread gravitational waves, energy-carrying waves through a gravitational area, which emerge from a huge body acceleration or disturbance.
The confrontation between the neutron stars has been the subject of many theoretical physics studies, as a deep understanding of these phenomena can achieve interesting insight on how substance behaves on extreme density. The behavior of the substance at extremely high density is currently described by a theoretical structure known as the state equation (EOS).
Recent Astrophysics Research has discovered the possibility that EOS features, such as phase transition or a quark-hidron crossover, can be estimated from the gravitational wave spectrum seen after the merger of neuron stars. However, most of these theoretical functions did not consider the effects of magnetic fields on this spectrum.
Researchers at the University of Urbana-Shampain and Valencia, the University of Illinois, recently performed a series of simulation, aimed at better understanding the impact of magnetic fields on the oscillation frequencies of Major Neutron Stars. Their paper, Published In Physical review paperThis indicates that the magnetic fields alone can also result in frequency innings, thus explaining the comments of the neutron star merger can be more challenging than the first anticipated.
“The next generation gravitational wave observatories, such as cosmic explorers, will be able to detect the actual merger of two neutron stars as they manufacture various frequencies of ingredients associated with a single rotating compact object and merger process,” Antonios Tsocaros, the prominent author of the paper, told Fiz.ORG.
“These frequencies encoded many characteristics of neutron stars. Therefore, by identifying them correctly, we will be able to understand many unknown qualities of these extraordinary objects.”
Neutron stars have two main features that are yet to be fully understood and make them attractive physical laboratories. First, they have unique thermodynamic properties, such as described by EOS, at its core. Due to these properties, just one teaspoon of neutron star content weighs as much as Mount Everest.
Another major feature of neutron stars is their magnetic field. During the Nutron Star merger, this magnetic field can reach a billion more values than the largest magnetic field created by humans.
The lower plot shows frequency shifts as a function of magnitude of magnetic field for the main oscillation mode in relation to the non -chambal case. Such frequency changes in the residue of the merger can occur for several reasons: 1) a phase infection or more, the existence of the presence of asymmetrical, non-respective dynamics. 2) The existence of a quarks of a quarks of a quarks of a state crossover equation. 3) finite temperature effects. 4) Strictness of state equation. 5) Out and out-balance effects, such as bulk viscosity. 6) Magnetic field. 7) Spin of pre -neutron stars. In addition to 6, 7 items in the list above, everything else is related to the state’s unknown equation, either in its cold or in its warm area. The horrors of predictive innings differ for each reason above, but overlap is important. This means that any shift estimated by 1-5 items can be masked by the magnetic field (or even pre-neutron star spin), and therefore any interpretation of observation data should be done with caution. Credit: Tsocaros et al.
“Our job systematically tries systematically to understand the impact of the magnetic field on the oscillation frequencies of the post-mentor neutron star and inform about various competitive effects,” Tsocaros said. “Previous work by other investigators has been highly optimistic at an attempt to identify thermodynamic properties in the interior of neutron stars, which is completely ignoring the effects coming from its magnetic field. On the other hand, we clearly show that this omission can be misleading, and that the magnetic field should be included for the correct interpretation of the reconciliation.
As part of his recent study, Tsocaros and his colleagues later demonstrated the general relative magnetohydrogenamics simulation to detect the effects of magnetic fields on the oscillation frequencies of the Meragar Neutron Stars. In these simulations, he used two neutron stars EOS, two different -nutron star mass and three different magnetic field topology.
“The magnetic field is enabled to large values during merger,” the Jamie Bumber explained the postdock working with professors Tsockeros and Shapiro. “Our simulation has shown that the strong magnetic field causes residue to the merger and produces gravitational waves at high frequency. This increase in frequency can mask the change of frequency from a different origin such as a change in EOS, the interpretation of potentially complicated.”
Professor Milton Ruiz said, “To accurately evaluate the post-magnificent phase in the binary neutron star merger, thus one needs to include the effects of the magnetic field. Failing to do so may lead to wrong conclusion about the physical properties of the system.”
Overall, this recent study suggests that the effects of magnetic fields can complicate the interpretation of gravitational wave data arising from the neutron star merger. In his future research, Tsokaros and his colleagues planned to confirm their recent results by demonstrating further simulation on their recent results on more resolutions that were previously computationally prohibited.
Professor Stuart L. Shapiro said, “Ligo was identified for the first time from the same cosmic source from the same cosmic source due to the identity of gravitational waves in 2017 and a gamma-raw by NASA satellites,” Professor Stuart L. Shapiro said.
“This marked a success in the multi-sensitive astronomy and at the University of Illinois, such as performing at the University of Illinois. Post-mosques of binary neutron stars.”
More information:
Antonios Tsocaros et al, Mask the equation-off-state effects in the binary neutron star merger, Physical review paper (2025). Doi: 10.1103/physrevlett.134.121401But arxiv, Doi: 10.48550/arxiv.2411.00939
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Citation: Rethinking Neutron Star merger: The study examines the effects of magnetic fields on their oscillation frequencies (2025, 20 April).
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