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Burdyuzha, V. V.; Kauts, V. L.

doi:10.1023/a:1001760029699

Cited by 6 publications

(13 citation statements)

References 17 publications

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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%

“…An only part of previous researches of Ps may be used to a dark Ps. In [13] we have shown that there is a power-law suppression of positronium formation in excited states relative to the ground state. The positronium H α (λ~1.3 μ) line, whose suppression factor is not so large (~1/n 3 ), is the most suitable line for detection toward the Galactic Center for usual Ps.…”

Section: A Laboratory Positroniummentioning

confidence: 88%

“…Thus, the Ps characteristic lines are the first lines of the Lyman L α (2431Å) n=2→n=1, Balmer H α (1.3 μ) n=3→n=2, Paschen P α (3.75 μ) n=4 →n=3, Brackett Br α (8.1 μ) n=5→n=4, Pfund Pf α (14.9 μ) n=6→n=5, Humphreys (24.7 μ) n=7→n=6 series, etc. Besides, in [14] we researched possibility of detecting the hyperfine ground state transition of positronum (λ~0.147 cm) under various astrophysical conditions. The maser effect may be also realizable.…”

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: 88%

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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“…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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“…Since most previous studies have focussed on the Galactic centre as the most promising source of Ps recombination line emission (so far the only source other than the Sun in which Ps annihilation has been observed) and that at the Galactic centre the visual extinction is very high, it is not surprising that this idea has remained largely forgotten. Burdyuzha & Kauts (1997) raised the possibility of optical/ IR detection of Ps again, and made predictions of the expected fluxes of the most important lines. However, the only published attempt to detect Ps recombination lines was made by Puxley & Skinner (1996) who searched for Ps Paschen-β from the Galactic centre in the K band, and whose non-detection provides the only direct experimental constraints on the emission.…”

Section: Introductionmentioning

confidence: 99%

The Search for Celestial Positronium via the Recombination Spectrum

Ellis

Bland-Hawthorn

2009

ApJ

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Positronium is the short-lived atom consisting of a bound electron-positron pair. In the triplet state, when the spins of both particles are parallel, radiative recombination lines will be emitted prior to annihilation. The existence of celestial positronium is revealed through gamma-ray observations of its annihilation products. These observations however have intrinsically low angular resolution. In this paper we examine the prospects for detecting the positronium recombination spectrum. Such observations have the potential to reveal discrete sources of e + for the first time and will allow the acuity of optical telescopes and instrumentation to be applied to observations of high energy phenomena.We review the theory of the positronium recombination spectrum and provide formulae to calculate expected line strengths from the e + production rate and for different conditions in the interstellar medium. We estimate the positronium emission line strengths for several classes of Galactic and extragalactic sources. These are compared to current observational limits and to current and future sensitivities of optical and infrared instrumentation. We find that observations of the Psα line should soon be possible due to recent advances in near-infrared spectroscopy.

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Untitled

Cited by 6 publications

References 17 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

Astrophysical signatures of leptonium

The Search for Celestial Positronium via the Recombination Spectrum

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Untitled

Cited by 6 publications

References 17 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

Astrophysical signatures of leptonium

The Search for Celestial Positronium via the Recombination Spectrum

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Resources

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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