Positronium in Astrophysical Condition

Burdyuzha, V. V.; Kauts, V. L.; Yudin, N. P.

doi:10.1007/978-94-011-2761-5_14

Cited by 3 publications

(6 citation statements)

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“…As seen from results of that paper in a plasma at small T (T<10 eV) recombination takes place, in general, to the 2P levels (see Fig. in our articles [8,[13][14]). The production of the L α -line has a probability of 15% with respect to that of the annihilation line (in number of photons), i.e.…”

Section: A Laboratory Positroniumsupporting

confidence: 57%

“…At first some worlds are necessary to say of "usual positronium" and it spectrum. A L α line of Ps (2431Å) is impossible to observe in the direction of Galactic Center because of the strong extinction takes place here [8] although a positron excess was also observed in this direction [7]. An obvious signature of positrons is the 511 keV annihilation lines which were observed in at least two celestial objects: solar flares and the Galactic Center [9].…”

Section: A Laboratory Positroniummentioning

confidence: 82%

“…The process of thermalization is strongly dependent on the physical state of the medium. In [8] we already analyzed the possibility of observation of the L α -line of Ps (λ~2431Å). As seen from results of that paper in a plasma at small T (T<10 eV) recombination takes place, in general, to the 2P levels (see Fig.…”

Section: A Laboratory Positroniummentioning

confidence: 99%

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Lα Line of Dark Positronium as a Nongravitational Detection of DM

Burdyuzha¹,

Charugin²

2015

JMP

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An attempt to predict the new atomic dark matter lines is done on the example of a dark lepton atompositronium. Its Layman-alpha line with the energy near 3 GeV may be observable if the appropriate conditions realize. For this we have studied a γ-ray excess in the Center of our Galaxy. In principle, this excess may be produced by the L α line of a dark positronium in the medium with Compton scattering. The possibility of observations of an annihilation line (E~300 TeV) of dark positronium is also predicted. Other proposals to observe the atomic dark matter are shortly described. Besides, H α line (1.3μ) of usual positronum must be observable in the direction on the Center of our Galaxy.

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Section: A Laboratory Positroniumsupporting

confidence: 57%

Section: A Laboratory Positroniummentioning

confidence: 82%

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Lα Line of Dark Positronium as a Nongravitational Detection of DM

Burdyuzha¹,

Charugin²

2015

JMP

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“…The curious possibility to explain the excess in the gamma-ray spectrum (1-3 GeV) from the Galactic center region by the L α line of dark Ps arises here. The L α line of ordinary Ps (2431Å) cannot be observed toward the center of our Galaxy due to strong absorption in the ultraviolet [65]. One might probably expect the development of dark-medium spectroscopy and, as a consequence, the non gravitational detection of dark matter.…”

Section: Dark Mattermentioning

confidence: 94%

The dark components of the Universe are slowly clarified

Burdyuzha

2017

J. Exp. Theor. Phys.

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The dark sector of the Universe is beginning to be clarified step by step. If the dark energy is vacuum energy, then 123 orders are exactly reduced by ordinary physical processes. For many years these unexplained orders were called a crisis in physics. There was indeed a "crisis" before the introduction of the holographic principle and entropic force in physics. The vacuum energy was spent for the organization of new microstates during the entire life of the Universe, but in the initial period of its evolution the vacuum energy (78 orders) were reduced more effectively by the vacuum condensates produced by phase transitions, because the Universe lost the high symmetry during its expansion. Important problems of physics and cosmology can be solved if the quarks, leptons, and gauge bosons are composite particles. The dark matter, partially or all consisting of familon-type pseudo-Goldstone bosons with a mass of 10 -5 -10 -3 eV, can be explained in the composite model. Three generations of elementary particles are absolutely necessary in this model. In addition, this model realizes three relativistic phase transitions in a medium of familons at different red shifts, forming a large-scale structure of dark matter that was "repeated" by baryons. We predict the detection of dark matter dynamics, the detection of familons as dark matter particles, and the development of spectroscopy for dark medium due to the probable presence of dark atoms in it. Other viewpoints on the dark components of the Universe are also discussed briefly.

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“…The first attempt to quantify the expected Ps recombination line strengths was made by McClintock (1984) [48], who was motivated by the planned space telescope, which was eventually to become the Hubble Space Telescope, and found that Lyman α emission from the Crab pulsar and NGC 4151 should be detectable in principle. The issue of detecting Ps recombination lines has subsequently been revisited several times [49,50,47,51], and most recently by the authors [52] based on recent advances in near infrared spectroscopy. So far, however, Ps recombination lines from astrophysical sources have escaped detection.…”

Section: Recombination Linesmentioning

confidence: 99%

Astrophysical signatures of leptonium

Ellis

Bland-Hawthorn

2018

Eur. Phys. J. D

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More than 10 43 positrons annihilate every second in the centre of our Galaxy yet, despite four decades of observations, their origin is still unknown. Many candidates have been proposed, such as supernovae and low mass X-ray binaries. However, these models are difficult to reconcile with the distribution of positrons, which are highly concentrated in the Galactic bulge, and therefore require specific propagation of the positrons through the interstellar medium. Alternative sources include dark matter decay, or the supermassive black hole, both of which would have a naturally high bulge-to-disc ratio. The chief difficulty in reconciling models with the observations is the intrinsically poor angular resolution of gamma-ray observations, which cannot resolve point sources. Essentially all of the positrons annihilate via the formation of positronium. This gives rise to the possibility of observing recombination lines of positronium emitted before the atom annihilates. These emission lines would be in the UV and the NIR, giving an increase in angular resolution of a factor of 10 4 compared to gamma ray observations, and allowing the discrimination between point sources and truly diffuse emission. Analogously to the formation of positronium, it is possible to form atoms of true muonium and true tauonium. Since muons and tauons are intrinsically unstable, the formation of such leptonium atoms will be localised to their places of origin. Thus observations of true muonium or true tauonium can provide another way to distinguish between truly diffuse sources such as dark matter decay, and an unresolved distribution of point sources. .Lx Recombination, attachment, and positronium formation -36.10k Exotic atoms and molecules -95.30.Cq Elementary particle processes -95.30.Ky Atomic and molecular data, spectra, and spectral parameters

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Positronium in Astrophysical Condition

Cited by 3 publications

References 2 publications

<i>L<sub>α</sub></i> Line of Dark Positronium as a Nongravitational Detection of DM

<i>L<sub>α</sub></i> Line of Dark Positronium as a Nongravitational Detection of DM

The dark components of the Universe are slowly clarified

Astrophysical signatures of leptonium

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Positronium in Astrophysical Condition

Cited by 3 publications

References 2 publications

&lt;i&gt;L&lt;sub&gt;α&lt;/sub&gt;&lt;/i&gt; Line of Dark Positronium as a Nongravitational Detection of DM

&lt;i&gt;L&lt;sub&gt;α&lt;/sub&gt;&lt;/i&gt; Line of Dark Positronium as a Nongravitational Detection of DM

The dark components of the Universe are slowly clarified

Astrophysical signatures of leptonium

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<i>L<sub>α</sub></i> Line of Dark Positronium as a Nongravitational Detection of DM

<i>L<sub>α</sub></i> Line of Dark Positronium as a Nongravitational Detection of DM