Start Date
5-9-2016 10:15 AM
End Date
5-9-2016 10:45 AM
Description
This poster will focus on the analysis of extinction spectra obtained from simulations of exoplanet atmospheres; these spectra have been simulated using a variety of particle types and size distributions. To simulate these spectra, we have created a MATLAB program that uses mathematical models and complex algorithms to model Mie and spherical scattering. This scattering of light from aerosols has been modeled in the ultraviolet to near infrared band (200-1100 nm). We have modeled atmospheric compositions that are typical of Jovian planets, using known information about the atmosphere of Jupiter (see our first poster, entitled “Direct Optical Detection of Microorganisms in Exoplanet Atmospheres: Methods”).
Extinction spectra were simulated for six particle types: Erwinia herbicola (EH), Bacillus atrophaeus (BG), ovalbumin (OV), ammonia ice, water, and water ice. Initial results show that the extinction spectra of microorganisms are distinctly different from those of water and ammonia ice clouds; all spectra resemble complex polynomial functions, but the size and location of the peaks vary according to the composition of the particles simulated. These differences are amplified when the size of the particles tested is proportional to the wavelength of the light.
There are many variables that could affect this change in extinction spectra. The resulting data from the simulations detailed above has been analyzed to determine which variables most affect the spectra. This analysis focused on the variation of four parameters: refractive index, average particle size, percent volume, and standard deviation.
Direct Optical Detection of Microorganisms in Exoplanet Atmospheres: Models & Results
This poster will focus on the analysis of extinction spectra obtained from simulations of exoplanet atmospheres; these spectra have been simulated using a variety of particle types and size distributions. To simulate these spectra, we have created a MATLAB program that uses mathematical models and complex algorithms to model Mie and spherical scattering. This scattering of light from aerosols has been modeled in the ultraviolet to near infrared band (200-1100 nm). We have modeled atmospheric compositions that are typical of Jovian planets, using known information about the atmosphere of Jupiter (see our first poster, entitled “Direct Optical Detection of Microorganisms in Exoplanet Atmospheres: Methods”).
Extinction spectra were simulated for six particle types: Erwinia herbicola (EH), Bacillus atrophaeus (BG), ovalbumin (OV), ammonia ice, water, and water ice. Initial results show that the extinction spectra of microorganisms are distinctly different from those of water and ammonia ice clouds; all spectra resemble complex polynomial functions, but the size and location of the peaks vary according to the composition of the particles simulated. These differences are amplified when the size of the particles tested is proportional to the wavelength of the light.
There are many variables that could affect this change in extinction spectra. The resulting data from the simulations detailed above has been analyzed to determine which variables most affect the spectra. This analysis focused on the variation of four parameters: refractive index, average particle size, percent volume, and standard deviation.