The abundances of heavy elements in BL138 – red giant of local group fornax dwarf spheroidal galaxy

Gopka, V. F.; Yushchenko, A. V.; Yushchenko, V. A.; Шаврина, А. В.; Andrievsky, S.; Jeong, Yeuncheol; Shereta, E. P.

doi:10.26577/phst-2018-1-146

Cited by 3 publications

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“…Òîáòî, åì³ñ³ÿ, õàðàêòåðíà äëÿ ñèëüíèõ ë³í³é, ÿêèìè º ë³í³¿ Ca II H&K, áóëà íàñë³äêîì ðîñòó òåìïåðàòóðè â íèae í³é ÷àñòèí³ àòìîñôåðè íà ïåâíèõ ïðîì³aeêàõ ÷àñó. Çíàéäåíà íàìè êîðåëÿö³ÿ ïîÿâè åì³ñ³éíèõ êîìïîíåíò³â ñèëüíèõ ë³í³é ó ñïåêòðàõ ç³ð ç ïîÿâîþ ë³í³é ðàä³îàêòèâíèõ åëåìåíò³â, çîêðåìà àêòèí³þ, ó ñïåêòðàõ ç³ð â ãàëàêòèêàõ ç ð³çíîþ ³ñòîð³ºþ çáàãà÷åííÿ, ÿê-òî â íàø³é Ãàëàêòèö³ (HD101065, [2]), êàðëèêîâ³é ãàëàêòèö³ Ôîðíàêñ (BL138) [11], Âåëèê³é Ìàãåëëàíîâ³é Õìàð³ (RM_1-667) [9], ìîaeóòü áóòè ä³éñíî ïîâ'ÿçàí³ ç «ãàðÿ÷îþ ìàòåð³ºþ â íèaeí³é ÷àñòèí³ àòìîñôåðè», ùî º âàaeëèâèì äëÿ ðîçóì³ííÿ ïðîöåñ³â, ÿê³ ïðîõîäÿòü â íåñòàá³ëüíèõ àòìîñôåðàõ.…”

Section: âñòóïunclassified

“…Àêòèí³é º òðåò³ì åëåìåíòîì, ïîðÿä ç òîð³ºì òà óðàíîì, ÿêèé íàëåaeèòü äî ãðóïè àêòèíî¿ä³â ³ ÿêèé äîñë³äaeóºòüñÿ â àòìîñôåðàõ ç³ð. Íàãàäàºìî, ùî àêòèí³é -ðàä³îàêòèâíèé åëåìåíò, ó ÿêîãî ³çîòîï ç íàéá³ëüøèì ïåð³îäîì ï³âðîçïàäó ñòàíîâèòü âñüîãî 21.772(3) ðîêè, óòâîðþºòüñÿ ïðè ðîçïàä³ ðàä³îàêòèâíîãî ðÿäó óðàíó 235 U. Ë³í³¿ ïîãëèíàííÿ àêòèí³þ íà äîâaeèíàõ õâèëü l 591.085 íì ³ l 616.475 íì, îòîòîaeíåí³ ó ñïåêòðàõ ÷åðâîíîãî íàäã³ãàíòà RM_1-667, ùî íàëåaeèòü Âåëèê³é Ìàãåëëàíîâ³é Õìàð³ [9] òà ó ñïåêòð³ ÷åðâîíîãî ã³ãàíòà BL138 [11], ùî íàëåaeèòü ñôåðî¿äàëüí³é êàðëèêîâ³é ãàëàêòèö³ Ôîðíàêñ, ìàþòü àíîìàëüíèé ïðî -ô³ëü âîäíþ ³ (àáî) ³íøèõ ñèëüíèõ ë³í³é. Äîñë³äaeåííÿ ë³í³é àêòè í³þ â îïòè÷í³é îáëàñò³ ñïåêòðó ç³ð RM_1-667 òà BL138 (Ôîðíàêñ), ÿê³ íå íàëåaeàòü äî íàéñèëüí³øèõ, ñïîíóêàëî íàñ çâåðíóòèñÿ äî ë³í³é àêòèí³þ ó êîðîòêîõâèëüîâ³é ÷àñòèí³ ñïåêòðó, äå, çã³äíî ç ëàáîðàòîð íèìè äîñë³äaeåííÿìè, ë³í³¿ àêòèí³þ º á³ëüø ³íòåíñèâíèìè.…”

Section: âèñíîâêè òà îáãîâîðåííß ðåçóëüòàò²âunclassified

“…Ìè âèçíà÷èëè âì³ñò àêòèí³þ (lgN(Ac) = -1.20) â àòìîñôåð³ öå -ôå¿äè HIP 13962, ÿêèé íå â³äð³çíÿºòüñÿ çíà÷íî â³ä âì³ñòó öüîãî åëåìåí òó â àòìîñôåð³ ÷åðâîíîãî íàäã³ãàíòà RM_1-667 Âåëèêèõ Ìàãåëëàíîâèõ Õìàð (lgN(Ac) = -1.30 [8]) ³ â àòìîñôåð³ ÷åðâîíîãî ã³ãàíòà BL138 (lgN(Ac) = -1.60 [11]). Àëå â àòìîñôåð³ çîð³ Ïøèáèëüñüêîãî âì³ñò àêòèí³þ á³ëüø í³ae íà äâà ïîðÿäêè âèùèé: lgN(Ac) = 0.94 ± 0.09 â øêàë³ lgN(H) = 12 [2].…”

Section: âèñíîâêè òà îáãîâîðåííß ðåçóëüòàò²âunclassified

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The Radioactive Elements in the Atmosphere of HD25354—Are They the Result of the Symmetric Decay of the Chemical Elements of the Island of Stability?

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In this research, we investigated the observed spectra of the hot peculiar star HD25354 with an effective temperature Teff = 12,800 K, identified the lines of radioactive chemical elements, including the elements with short decay time, and estimated the abundances of these elements. We tried to confirm or reject the existence of promethium lines and lines of other radioactive elements which were detected in previous investigations of this star and explain the physical mechanisms which are responsible for the synthesis of these elements in the stellar atmosphere. We used two high-dispersion spectra of HD25354 observed with the 2 m telescope of Terskol observatory with resolving power near R = 60,000, and a signal to noise ratio near 200. The spectrum of the star from the archive of the 1.93 m telescope of Haute-Provence observatory was also used. The observations were compared with synthetic spectra and the abundance of promethium was found using the best four lines of this element in the observed spectra: logN(Pm) = 5.84 ± 0.16 in the scale logN(H) = 12. It is comparable to the abundances of stable lanthanides in the atmosphere of this star. The abundance of thorium derived from two lines of double-ionized thorium is logN(Th) = 3.59 ± 0.15. The upper limits for technetium, radium, actinium, uranium, and americium abundances are found to be equal to 4.0, 3.0, 1.25, 3.5, and 4.0, respectively. Maybe the existence of promethium lines and lines of other unstable chemical elements in the spectra of HD25354, as well as the other stars of our Galaxy, Magellanic Clouds, and Fornax dwarf galaxy, can be explained by contamination of its atmosphere by the products of kilonova outburst and by symmetric decay of chemical elements with long decay times located at the island of stability (atomic numbers Z = 110–128) of transfermium elements. Maybe the decay of superheavy elements of the island of stability can be one of the reasons for the enhanced abundances of rare earth lanthanides in different types of stars.

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The abundances of heavy elements in BL138 – red giant of local group fornax dwarf spheroidal galaxy

Cited by 3 publications

References 0 publications

Analysis of actinium abundances in the atmosphere of Cepheid HIP13962

Analysis of actinium abundances in the atmosphere of Cepheid HIP13962

Analysis of Actinium Abundances in the Atmosphere of Cepheid HIP13962

The Radioactive Elements in the Atmosphere of HD25354—Are They the Result of the Symmetric Decay of the Chemical Elements of the Island of Stability?

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