Accumulative coupling between magnetized tenuous plasma and gravitational waves

Zhang, Fan

doi:10.1103/physrevd.94.024048

Cited by 3 publications

(2 citation statements)

References 50 publications

(85 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…On the other hand, according to contemporary observations, there are very widespread background galactic magnetic fields (GMFs, strength around ∼ 10 −10 to 10 −9 Tesla) [28] within the Milky way. Therefore, according to the electrodynamics in curved spacetime, in the frame of EM response to GWs, we propose that such high-frequency GWs of sub-solar mass PBH binary mergers will interact with the GMFs in the Milky The effect of EM response to GWs had been long studied [29][30][31][32][33][34][35][36][37][38][39][40][41][42][43][44][45][46], and previous works [30,[35][36][37]45] indicated that the strengths of perturbed EMWs depends on both strengths and spatial scales (accumulation distance) of the background magnetic fields. Thus, the GMFs will provide a huge accumulation distance to compensate the weakness of their very low strengths, and then would lead to considerable EM signals.…”

Section: Introductionmentioning

confidence: 99%

Distinctive electromagnetic signals caused by gravitational waves (of sub-solar mass primordial black hole binary mergers) interacting with galactic magnetic fields

Wen¹

2019

Preprint

View full text Add to dashboard Cite

As a candidate of dark matter, and related to many fundamental physics issues, the primordial black hole (PBH) is a crucial topic. However, so far the existence of PBHs is still not confirmed, and currently running gravitational wave (GW) detectors are still not able to distinguish them from the normal astrophysical black holes. In this article, we propose that the GWs (of PBH binary mergers) could interact with the very widespread background galactic magnetic fields in the Milky way, to produce the perturbed electromagnetic waves (EMWs) with unique characteristics of frequencies, waveforms, spectra and polarizations. In order to be distinguished from astrophysical black holes, only the PBHs with masses less than the solarmass are considered here, and their binary mergers will radiate GWs in frequencies much higher above the plasma frequency of interstellar medium (ISM), so corresponding perturbed EMWs (in the same frequencies to such GWs) can propagate through the ISM until the Earth. Our estimations show that, for the sub-solar mass PBH binary mergers within the Milky way (disk or halo), the strengths of the perturbed EMWs turn into constant levels around ∼ 10 −12 Tesla (for magnetic components) and ∼ 10 −10 W att • m −2 (for energy flux densities) at the Earth, generally for all cases of different PBH masses (and not dependent on the distance of sources), and the same mass ratio of the PBH binary gives the same strength (at the Earth) of perturbed EMWs despite different PBH masses (GW frequencies) or binary distances. Differently, for the sub-solar mass PBH binary mergers outside the Milky way, the perturbed EMWs at Earth have lower strengths (and depend on the distance of sources), but for some part of distance range, they would also be detectable. If such EM signals and special EM counterpart of GWs from PBHs could be detected by space-or land-based EMWs detectors, it may provide direct evidence of the PBHs.

show abstract

Section: Introductionmentioning

confidence: 99%

Distinctive electromagnetic signals caused by gravitational waves (of sub-solar mass primordial black hole binary mergers) interacting with galactic magnetic fields

Wen¹

2019

Preprint

View full text Add to dashboard Cite

show abstract

“…proposed here based on the effect of EM response to GWs, which had been long studied [23][24][25][26][27][28][29][30][31][32][33][34][35][36][37][38][39][40] but were usually in very high frequency bands such as over GHz (10 9 Hz) [28][29][30][31][32][33][34][35][36][37][38][39]. Whereas, we now apply such mechanism targeting on the GWs in the intermediate band (around ∼ 10 1 to ∼ 10 3 Hz) from the binary mergers.…”

mentioning

confidence: 99%

Ultra-low-frequency electromagnetic waves as signals and special counterparts of gravitational waves (from binary mergers) having tensorial and possible nontensorial polarizations

Wen¹

2018

Preprint

View full text Add to dashboard Cite

Gravitational waves (GWs, from binary merger) interacting with super-strong magnetic fields of the neutron star (in the same binary system), would lead to perturbed electromagnetic waves [EMWs, in the same frequencies of these GWs, partially in the ultra-low-frequency (ULF) band for the EMWs]. Such perturbed ULF-EMWs are not only the signals, but also a new type of special EM counterparts of the GWs (unlike usual EM counterparts of gamma-ray bursts, they have accurately the same start time to the GWs). Here, generation of the perturbed ULF-EMWs is investigated, and the strengths of their magnetic components are estimated to be around 10 −12 Tesla to 10 −17 Tesla at the Earth for various cases, which would be already within or approaching the sensitivity range of the cutting-edge technologies of the magnetometry. Especially, for the case that the neutron star in the binary is a magnetar, the strengths of signals with level of ∼ 10 −13 to ∼ 10 −15 Tesla are already detectable by current highly sensitive ULF detectors and magnetometers. Waveforms of the perturbed ULF-EMWs will be modified into shapes different but related to the waveforms of the GWs, due to the amplification process during the binary mergers which could amplify the magnetic fields into 10 12 Tesla or even higher. Specific connection relationships between the polarizations of the perturbed ULF-EMWs and the polarizations (tensorial and possible nontensorial) of the GWs of binary mergers, are also addressed. These characteristic waveforms and particular polarizations of the perturbed ULF-EMWs will be very helpful for filtering and extracting the signals from background noise. Briefly, we propose such a potential novel way of detection for signals and special EM counterparts of the GWs from binary mergers, which would bring us some different new information of fundamental properties of the gravity and Universe that other GW detections may not provide.

show abstract

On the transverse-traceless gauge condition when matter is presented

Xue,

He,

Cao

2024

Commun. Theor. Phys.

View full text Add to dashboard Cite

The transverse-traceless gauge condition is an important concept in the theory of gravitational wave. It is well known that vacuum is one of the key conditions to guarantee the existence of the transverse-traceless gauge. Although it is thin, interstellar medium is ubiquitous in the universe. Therefore, it is important to understand the concept of gravitational wave when matter is presented. Bondi-Metzner-Sachs theory has solved the gauge problem related to gravitational wave. But it does not help with the cases when gravitational wave propagates in matters. This paper discusses possible extensions of the transverse-traceless gauge condition to Minkowski perturbation with matter presented.

show abstract

Accumulative coupling between magnetized tenuous plasma and gravitational waves

Cited by 3 publications

References 50 publications

Distinctive electromagnetic signals caused by gravitational waves (of sub-solar mass primordial black hole binary mergers) interacting with galactic magnetic fields

Distinctive electromagnetic signals caused by gravitational waves (of sub-solar mass primordial black hole binary mergers) interacting with galactic magnetic fields

Ultra-low-frequency electromagnetic waves as signals and special counterparts of gravitational waves (from binary mergers) having tensorial and possible nontensorial polarizations

On the transverse-traceless gauge condition when matter is presented

Contact Info

Product

Resources

About