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X-ray signature of antistars in the Galaxy. / Bondar, A. E.; Blinnikov, S. I.; Bykov, A. M. et al.

In: Journal of Cosmology and Astroparticle Physics, Vol. 2022, No. 3, 009, 03.2022.

Research output: Contribution to journal › Article › peer-review

Harvard

Bondar, AE, Blinnikov, SI, Bykov, AM, Dolgov, AD & Postnov, KA 2022, 'X-ray signature of antistars in the Galaxy', Journal of Cosmology and Astroparticle Physics, vol. 2022, no. 3, 009. https://doi.org/10.1088/1475-7516/2022/03/009

APA

Bondar, A. E., Blinnikov, S. I., Bykov, A. M., Dolgov, A. D., & Postnov, K. A. (2022). X-ray signature of antistars in the Galaxy. Journal of Cosmology and Astroparticle Physics, 2022(3), [009]. https://doi.org/10.1088/1475-7516/2022/03/009

Vancouver

Bondar AE, Blinnikov SI, Bykov AM, Dolgov AD, Postnov KA. X-ray signature of antistars in the Galaxy. Journal of Cosmology and Astroparticle Physics. 2022 Mar;2022(3):009. doi: 10.1088/1475-7516/2022/03/009

Author

Bondar, A. E. ; Blinnikov, S. I. ; Bykov, A. M. et al. / X-ray signature of antistars in the Galaxy. In: Journal of Cosmology and Astroparticle Physics. 2022 ; Vol. 2022, No. 3.

BibTeX

@article{0f8f62813e374d6ea222de8c5525ea59,
title = "X-ray signature of antistars in the Galaxy",
abstract = "The existence of macroscopic objects from antimatter (antistars) is envisaged in some models of baryogenesis. Searches for antistars have been usually carried out in gamma-rays originated from hadronic annihilation of matter. In astrophysically plausible cases of the interaction of neutral atmospheres or winds from antistars with ionized interstellar gas, the formation of excited pp¯ and Hep¯ atoms precedes the hadronic annihilation. These atoms rapidly cascade down to low levels before annihilation giving rise to a series of narrow lines which can be associated with the hadronic annihilation gamma-ray emission. The most significant are L (3p-2p) 1.73 keV line (yield more than 90%) from pp¯ atoms, and M (4-3) 4.86 keV (yield ∼60%) and L (3-2) 11.13 keV (yield about 25%) lines from 4Hep¯ atoms. These lines can be searched for in dedicated observations by the forthcoming sensitive X-ray spectroscopic missions XRISM, Athena and Lynx and in wide-field X-ray surveys like SRG/eROSITA all-sky survey.",
keywords = "baryon asymmetry, stars, X-rays",
author = "Bondar, {A. E.} and Blinnikov, {S. I.} and Bykov, {A. M.} and Dolgov, {A. D.} and Postnov, {K. A.}",
note = "Publisher Copyright: {\textcopyright} 2022 IOP Publishing Ltd and Sissa Medialab.",
year = "2022",
month = mar,
doi = "10.1088/1475-7516/2022/03/009",
language = "English",
volume = "2022",
journal = "Journal of Cosmology and Astroparticle Physics",
issn = "1475-7516",
publisher = "IOP Publishing Ltd.",
number = "3",

}

RIS

TY - JOUR

T1 - X-ray signature of antistars in the Galaxy

AU - Bondar, A. E.

AU - Blinnikov, S. I.

AU - Bykov, A. M.

AU - Dolgov, A. D.

AU - Postnov, K. A.

N1 - Publisher Copyright: © 2022 IOP Publishing Ltd and Sissa Medialab.

PY - 2022/3

Y1 - 2022/3

N2 - The existence of macroscopic objects from antimatter (antistars) is envisaged in some models of baryogenesis. Searches for antistars have been usually carried out in gamma-rays originated from hadronic annihilation of matter. In astrophysically plausible cases of the interaction of neutral atmospheres or winds from antistars with ionized interstellar gas, the formation of excited pp¯ and Hep¯ atoms precedes the hadronic annihilation. These atoms rapidly cascade down to low levels before annihilation giving rise to a series of narrow lines which can be associated with the hadronic annihilation gamma-ray emission. The most significant are L (3p-2p) 1.73 keV line (yield more than 90%) from pp¯ atoms, and M (4-3) 4.86 keV (yield ∼60%) and L (3-2) 11.13 keV (yield about 25%) lines from 4Hep¯ atoms. These lines can be searched for in dedicated observations by the forthcoming sensitive X-ray spectroscopic missions XRISM, Athena and Lynx and in wide-field X-ray surveys like SRG/eROSITA all-sky survey.

AB - The existence of macroscopic objects from antimatter (antistars) is envisaged in some models of baryogenesis. Searches for antistars have been usually carried out in gamma-rays originated from hadronic annihilation of matter. In astrophysically plausible cases of the interaction of neutral atmospheres or winds from antistars with ionized interstellar gas, the formation of excited pp¯ and Hep¯ atoms precedes the hadronic annihilation. These atoms rapidly cascade down to low levels before annihilation giving rise to a series of narrow lines which can be associated with the hadronic annihilation gamma-ray emission. The most significant are L (3p-2p) 1.73 keV line (yield more than 90%) from pp¯ atoms, and M (4-3) 4.86 keV (yield ∼60%) and L (3-2) 11.13 keV (yield about 25%) lines from 4Hep¯ atoms. These lines can be searched for in dedicated observations by the forthcoming sensitive X-ray spectroscopic missions XRISM, Athena and Lynx and in wide-field X-ray surveys like SRG/eROSITA all-sky survey.

KW - baryon asymmetry

KW - stars

KW - X-rays

UR - http://www.scopus.com/inward/record.url?scp=85126468348&partnerID=8YFLogxK

UR - https://www.mendeley.com/catalogue/3e31eb53-ff26-3e93-8e85-afc6316c3cb2/

U2 - 10.1088/1475-7516/2022/03/009

DO - 10.1088/1475-7516/2022/03/009

M3 - Article

AN - SCOPUS:85126468348

VL - 2022

JO - Journal of Cosmology and Astroparticle Physics

JF - Journal of Cosmology and Astroparticle Physics

SN - 1475-7516

IS - 3

M1 - 009

ER -

ID: 35726923