Oczekiwany rozkład deuteru międzygwiazdowego w heliosferze

Tarnopolski, S.

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Tytuł artykułu

Oczekiwany rozkład deuteru międzygwiazdowego w heliosferze

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Tarnopolski S.

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Warianty tytułu

The expected distribution of interstellar deuterium in the heliosphere

Języki publikacji

Abstrakty

Deuter jest istotnym źródłem wiedzy o historii i przyszłości Wszechświata oraz różnych procesach astrofizycznych zachodzących w Galaktyce. Przedmiotem badań niniejszej pracy jest neutralny deuter pochodzenia międzygwiazdowego obecny w heliosferze w postaci gazowej. Pomiary rozkładu neutralnego deuteru w fazie gazowej prowadzone metodami astrofizycznymi obarczonymi dużymi niepewnościami. W chwili obecnej istnieje możliwość zweryfikowania tych wyników przez pomiary in situ, prowadzone w heliosferze przez misję ULYSSES bądź też przez nadchodzącą misję IBEX. W literaturze, poza jedyną znaną pracą z końca lat 70-tych, brak jest danych dotyczących rozkładu neutralnego deuteru międzygwiazdowego w bliskiej heliosferze. Celem pracy było zbadanie obfitości neutralnego deuteru międzygwiazdowego w stosunku do neutralnego wodoru w heliosferze oraz rozpoznanie możliwości obserwacyjnych pod kątem obecnych lub przyszlych misji kosmicznych. W tym celu zbudowano od podstaw teoretyczny model rozkładu neutralnego deuteru i wodoru pochodzenia międzygwiazdowego w heliosferze, wykorzystujący najnowsze modele ciśnienia promieniowania w linii Lyman-α oraz pola jonizacji i za jego pomocą badano podobieństwa i różnice w rozkładzie obu gazów. Model teoretyczny rozkładu gazu opiera się na teorii kinetycznej, w której gaz jest opisywany przez funkcję rozkładu prędkości bedącą funkcją siedmiu zmiennych niezależnych: trzech współrzędnych przestrzennych, trzech współrzędnych w przestrzeni fazowej prędkości i czasu. Momenty funkcji rozkładu tj. gęstość gazu, prędkość masową oraz rozmycie termiczne uzyskuje się przez odpowiednie całkowanie funkcji rozkładu po przestrzeni prędkości. Rezultaty symulacji numerycznych prowadzą do następujących wniosków: na skutek różnic w ciśnieniu promieniowania działającego na atomy deuteru i wodoru należy spodziewać się wzrostu obfitości D/H w głąb heliosfery w stosunku do wartości w lokalnym obłoku międzygwiazdowym oraz przyspieszania deuteru w stosunku do wodoru aż do ok. 50% w pobliżu Słońca, co przekłada się na pond czterokrotnie większą energię atomów deuteru w stosunku do atomów wodoru. Wyniki to dają nadzieje na bezpośrednią detekcję neutralnego deuteru pochodzenia międzygwiazdowego w otoczeniu Słońca.

Deuterium is an important source of knowledge about the history and future of the Universe and the various astrophysical processes taking place in the Galaxy. The subject of this research work is the neutral deuterium of interstellar origin presented in the heliosphere in the gaseous form. Measurements of the neutral deuterium distribution in the gas phase are carried out by the astrophysical methods cursed with large uncertainties. At present, it is possible to verify these results by in situ measurements carried out in the heliosphere by the Ulysses mission, or by the forthcoming IBEX mission. In the literature, apart from the only known work from the end of 70th decade, there is no data on the distribution of neutral interstellar deuterium in the nearby heliosphere. The purpose of this study was to examine the abundance of neutral interstellar deuterium in relation to neutral hydrogen in the heliosphere and recognition of observation opportunities for present or future space missions. To this end, the theoretical distribution model of neutral interstellar deuterium and hydrogen in the heliosphere was built from scratch, using the latest models of radiation pressure in the Lyman-a line and ionization field and by means of it the similarities and differences in the distribution of the two gases were studied. Theoretical model of gas distribution is based on the kinetic theory, in which the gas is described by the velocity distribution function as a function of seven independent variables: three spatial coordinates, three coordinates in the velocity phase space and tim The moments of distribution functions such as gas density, bulk velocity and thermal spread are obtained by integrating the distribution function in the velocity space. The results of numerical simulations are the following due to the differences in the radiation pressure acting on the hydrogen and deuterium atoms, the abundance of D/H is expected to increase deep into the heliosphere in relation to its value in the local interstellar cloud and acceleration of deuterium in relation to hydrogen up to about 50% in the vicinity of the Sun, which translates into more than four times greater energy of the deuterium atoms in relation to hydrogen atoms. These results give hope for the direct detection of neutral interstellar deuterium in the vicini>of the Sun.

Słowa kluczowe

heliosfera rozkład deuteru międzygwiezdnego

heliosphera distribution interstellar deuterium in the heliosphere

Wydawca

Wydawnictwa Naukowe Instytutu Lotnictwa

Czasopismo

Prace Instytutu Lotnictwa

Rocznik

2009

Tom

Nr 2 (197)

Strony

111--272

Opis fizyczny

Bibliogr. 216 poz., rys., tab., wzory

Twórcy

autor

Tarnopolski S.

Instytut Lotnictwa

Bibliografia

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