Modelling of spectra with and without dust from Martian surface based on infrared data

• Autorzy: Zalewska N.

Identyfikatory

DOI

10.5604/05096669.1226928

Warianty tytułu

PL

Modelowanie widm zapylonych i niezapylonych znad marsjańskich powierzchni na podstawie pozyskanych widm w podczerwieni

• Języki publikacji: EN

Abstrakty

EN

This article aims to show mineral composition of Mars surface based on TES spectra (Thermal Emission Spectrometer-Mars Global Surveyor), measured in infrared thermal range. It presents how, based on TES data, spectra from selected Martian regions were modelled and interpreted after prior removal of atmospheric influences from the spectra using the Radiative Transfer Algorithm and Deconvolution Algorithm. The spectra from dark area of Cimmeria Terra and light Isidis Planitia were elaborated in cited publications. In the case of light areas ex. Arsia Mons, spectrum of dusty weathered surface of Mars was obtained (also after removal of atmospheric influences) from averaging spectra of dusty regions of Mars. Those aforementioned spectra were used in modelling Martian surface aiming to determine their mineral composition. Deconvolution Algorithm was chosen from the mentioned methods as a tool for the modelling. The spectra described above were used for the Martian surface modelling, such as the Hellas Basin and Martian meteorites SNC (Shergottites, Nakhlites, Chassignites), in order to determine their mineral composition. As a modelling tool one of the following methods of deconvolution algorithm can be chosen. Spectra for the modelling were obtained from the PFS spectrometer (Planetary Fourier Spectrometer) - (Mars Express) and mineralogical composition of basalts from the southern part of Poland were used for this purpose. The method of modelling which was used to determine the mineral composition of Mars and dust can be used in determining mineral composition of selected areas on the Earth from aerial and satellite levels, e.g., soil and vegetation with the use of spectral libraries and spectra of individual plant species.

PL

Artykuł opisuje próbę przybliżenia składu mineralogicznego powierzchni Marsa na podstawie gotowych widm z TES (Thermal Emission Spectrometer-Mars Global Surveyor), zmierzonych w podczerwieni, w zakresie termalnym. Przedstawione tu będzie, jak na podstawie danych z TES zostały modelowane i zinterpretowane widma z wybranych terenów Marsa po uprzednim oddzieleniu wkładu atmosfery od całości widma, algorytmami: transferu promieniowania (Radiative Transfer Algorithm) i dekonwolucji (Deconvolution Algorithm). W cytowanych publikacjach opracowano widma z ciemnego obszaru Cimmeria Terra i obszaru jasnego - Isidis Planitia . W przypadku obszarów jasnych, przykładowo obszar Arsia Mons, widmo zapylonej i zwietrzałej powierzchni Marsa zostało uzyskane (również po oddzieleniu wpływu atmosfery) z uśrednienia widm pochodzących z terenów o wysokim zapyleniu. Te opisane powyżej widma zostały wykorzystane do modelowania powierzchni marsjańskich, takich jak basen Hellas oraz meteoryty marsjańskie SNC, w celu ustalenia ich składu mineralnego. Jako narzędzie modelowania wybrano jedną z wymienionych metod Deconvolution Algorithm. Widma do własnego modelowania były pozyskane ze spektrometru PFS (Planetary Fourier Spectrometer)-(Mars Express) oraz wykorzystano w tym celu skład mineralogiczny bazaltów z południowej części Polski.

Słowa kluczowe

EN

Mars; deconvolution algorithm; infrared spectrometry; Martian dust; spectra modelling

PL

Mars; algorytm dekonwolucji; spektrometria w podczerwieni; pył marsjański; modelowanie widm

• Wydawca: Wydawnictwa Naukowe Instytutu Lotnictwa
• Czasopismo: Prace Instytutu Lotnictwa
• Rocznik: 2016
• Tom: Nr 4 (245)
• Strony: 287--308
• Opis fizyczny: Bibliogr. 21 poz.., rys., tab., wykr., wzory

Twórcy

autor

Zalewska N.

• Space Technologies Division, Institute of Aviation, Al. Krakowska 110/114, 02-256 Warsaw
• Space Research Centre, Polish Academy of Sciences, ul. Bartycka 18A, 00-716 Warsaw

Bibliografia

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