Atmospheric Model vs StellarRAD

The app uses a simple radiative transfer model for a planet with two leaky* atmospheric layers. It begins by calculating Te, the emission temperature of the planet by using the Solar constant and planetary Albedo. Te is called the Blackbody temperature because it is inferred by fitting a Blackbody curve to the observed outbound LWIR radiation. You can choose any of the 9 planets in our solar system, or choose one of your own making. The app then uses 5 parameters for the chosen “base” planet: the Albedo (alpha), distance from the sun (r), extinction coefficients of two atmospheric layers (epsilon1, 2), and the solar constant S0 to calculate temperatures and radiative flux densities. One can modify these 5 adjustable parameters from their base values, and update the result. A flux diagram is generated showing the incoming short wavelength (SW), and outgoing long wavelength (LW) radiation. Two model run results can be saved and differences displayed. Also, runs can be saved to a .csv file for E-mail export and spreadsheet analysis. Calculate the “natural” 33K greenhouse effect (compare Earth with and without an atmosphere), or change the extinction coefficients to see the effect of adding or reducing absorbing gasses. Predict what Mars might be like with an atmosphere, or see what would happen if the characteristics of our sun, albedo or planetary orbit change. This simple model can create hours of fun. The base parameter values for Earth nicely calculate Ts, Te, and T1 (upper troposphere) values, and the model correctly predicts Te’s for all the planets. INSTRUCTIONS: Load app, choose a “base” planet, segue with Update. Click Update to calculate the temperatures and flux densities. Segue to inspect the flux densities, and/or modify the base parameters to see changes. Save and compare differences in 2 runs. (C/C0) values are in CO2 equivalents. Save runs to .csv file for spreadsheet analysis. USAGE TIPS: Start with a base planet, but realize this simple 2 layer model cannot accurately predict the surface temperatures of the gas giants or Venus. Pressing the Back button allows you to refresh your parameter or base planet choices. Remember a 5 K change in Ts resulted in the Earth’s last Ice Age! For convenience, the Test planet can be used to create your own set of parameters without entering a planet name. Increasing the solar constant increases all temperatures. Increasing epsilon does nothing to Te, which depends only on S0, r, and alpha. Press On/Off & Home takes flux diagram screenshot. It is easy to remove a saved data file run (row) after import to spreadsheet. RADIATIVE FORCING and CLIMATE SENSITIVITY: Radiative forcing (dF) can be used to estimate the change in surface temperature (dTs) arising from that forcing using: dTs = lambda x dF, where lambda is the Climate Sensitivity in K / (W/m2). Forcing due to an atmospheric greenhouse gas such as CO2 can be expressed as: dF (in W/m2) = 5.35 × ln (C/C0), where C is the CO2 concentration [CO2] and C0 is the initial concentration (in ppm). For a single atmospheric layer Earth, changing the base value of epsilon = 0.78 to epsilon = 0.83 (d-epsilon = 0.05) gives an 3K T rise; roughly the equivalent of doubling [CO2] (and a forcing of 3.71 W/m2). There has been a [CO2] increase between the years 1750 (280 ppm) and 2000 (380 ppm). Thus dF = 5.35 x ln (370/280) = 1.5 W/m2. dTs = lambda x dF = 0.8 (K/(W/m2)) x 1.5 (W/m2) = 1.2 K over that timeframe (d-epsilon 0.02 used). * Leaky implies epsilon less than 1.

The StellarRAD App for all WiFi enabled StellarNet spectrometers makes real-time light measurement quick and easy. Acquire full spectrum analysis of LEDs, lamps, lasers, solar/ grow lights, & just about any type of luminaire from ultra-violet through the visible and near-infrared! This intuitive app lets users control their spectrometer and capture basic and more advanced light measurement parameters such as spectral irradiance and lumens. Colorimetric analysis such as CRI (color rendering index), CCT (correlated color temperature), xy chromaticity, and much more. Easily save and export your data and full spectral graph as .IRR text data file, screenshot, and/or PDF report with all parameters listed.