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 <front>
  <journal-meta>
   <journal-id journal-id-type="publisher-id">Journal of Natural Sciences Research</journal-id>
   <journal-title-group>
    <journal-title xml:lang="en">Journal of Natural Sciences Research</journal-title>
    <trans-title-group xml:lang="ru">
     <trans-title>Журнал естественнонаучных исследований</trans-title>
    </trans-title-group>
   </journal-title-group>
   <issn publication-format="print">2500-0489</issn>
   <issn publication-format="online">2500-0489</issn>
  </journal-meta>
  <article-meta>
   <article-id pub-id-type="publisher-id">96787</article-id>
   <article-categories>
    <subj-group subj-group-type="toc-heading" xml:lang="ru">
     <subject>Астрофизика</subject>
    </subj-group>
    <subj-group subj-group-type="toc-heading" xml:lang="en">
     <subject>Astrophysics</subject>
    </subj-group>
    <subj-group>
     <subject>Астрофизика</subject>
    </subj-group>
   </article-categories>
   <title-group>
    <article-title xml:lang="en">Manifestations of shock waves around the halos of satellite galaxies and high-velocity clouds in the Galactic corona</article-title>
    <trans-title-group xml:lang="ru">
     <trans-title>Проявления ударных волн вокруг гало галактик – спутников и высокоскоростных облаков в короне Галактики</trans-title>
    </trans-title-group>
   </title-group>
   <contrib-group content-type="authors">
    <contrib contrib-type="author">
     <name-alternatives>
      <name xml:lang="ru">
       <surname>Поройков</surname>
       <given-names>С. Ю.</given-names>
      </name>
      <name xml:lang="en">
       <surname>Poroikov</surname>
       <given-names>Sergey Yu.</given-names>
      </name>
     </name-alternatives>
     <email>sporoykov@mail.ru</email>
     <bio xml:lang="ru">
      <p>кандидат физико-математических наук;</p>
     </bio>
     <bio xml:lang="en">
      <p>candidate of physical and mathematical sciences;</p>
     </bio>
     <xref ref-type="aff" rid="aff-1"/>
    </contrib>
   </contrib-group>
   <aff-alternatives id="aff-1">
    <aff>
     <institution xml:lang="ru">Московский государственный университет имени М.В.Ломоносова</institution>
    </aff>
    <aff>
     <institution xml:lang="en">Lomonosov Moscow State University</institution>
    </aff>
   </aff-alternatives>
   <pub-date publication-format="print" date-type="pub" iso-8601-date="2025-03-26T00:00:00+03:00">
    <day>26</day>
    <month>03</month>
    <year>2025</year>
   </pub-date>
   <pub-date publication-format="electronic" date-type="pub" iso-8601-date="2025-03-26T00:00:00+03:00">
    <day>26</day>
    <month>03</month>
    <year>2025</year>
   </pub-date>
   <volume>10</volume>
   <issue>2</issue>
   <fpage>2</fpage>
   <lpage>26</lpage>
   <self-uri xlink:href="https://zh-szf.ru/en/nauka/article/96787/view">https://zh-szf.ru/en/nauka/article/96787/view</self-uri>
   <abstract xml:lang="ru">
    <p>УФ линии поглощения в спектрах квазаров в короне галактики Андромеда показывают, что в пределах ≤0,15 Мпк горячий газ (~3∙105 К) содержит динамичную фракцию теплого газа (~104 К), связанную с ударными волнами (УВ). УВ формируются вокруг гало галактик – спутников размером ≤15 кпк и образуемых ими высокоскоростных облаков размером 2 – 15 кпк суммарной массой ~7∙109 М○, оседающих в Галактику ~109 лет, покрывая до 37% неба. Суммарная мощность УВ ~2∙1042 эрг/с излучается в виде УФ, рентгеновского и γ-излучения, а также космических лучей, электроны в которых (≥100 МэВ) тормозит магнитное поле МГД турбулентностей УВ 3 – 7 мкГс, образуя ГГЦ синхротронное радиоизлучение. Субкосмические лучи (электроны ≤100 кэВ) могут нагревать корональный газ (излучающий в области ~0,3 кэВ) и формировать тормозное излучение в области ~30 кэВ. Данные виды излучения в эпоху оседания мелких галактик в коронах более крупных при z ~ 0,45 ± 0,15 могут вносить вклад в фоновое космическое излучение с суммарной плотностью энергии ~10-4 эВ/см3.</p>
   </abstract>
   <trans-abstract xml:lang="en">
    <p>UV absorption lines in the spectra of quasars in the corona of the Andromeda galaxy show that within ≤0.15 Mpc the hot gas (~3∙105 K) contains a dynamic fraction of warm gas (~104 K) associated with shock waves (SW). SW are formed around the halos of satellite galaxies ≤15 kpc in size and the high-velocity clouds they form, 2–15 kpc in size, with a total mass of ~7∙109 M○, settling into the Galaxy in ~109 years, covering up to 37% of the sky. The total power of the SW of ~2∙1042 erg/s is emitted in the form of UV, X-ray and gamma radiation, as well as cosmic rays, the electrons in which (≥100 MeV) are braked by the magnetic field of MHD turbulences of the SW of 3 – 7 μG, forming GHz synchrotron radio emission. Subcosmic rays (electrons ≤100 keV) can heat the coronal gas (emitting at ~0.3 keV) and form bremsstrahlung in the region of ~30 keV. These types of radiation from the era of settling of small galaxies in the coronas of larger ones at z ~ 0.45 ± 0.15 can contribute to the background cosmic radiation with a total energy density of ~10-4 eV/cm3.</p>
   </trans-abstract>
   <kwd-group xml:lang="ru">
    <kwd>короны галактик</kwd>
    <kwd>высокоскоростные облака</kwd>
    <kwd>ударные волны в плазме</kwd>
   </kwd-group>
   <kwd-group xml:lang="en">
    <kwd>galactic coronas</kwd>
    <kwd>high-velocity clouds</kwd>
    <kwd>plasma shock waves</kwd>
   </kwd-group>
  </article-meta>
 </front>
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