Astrophysics and Python

Parameters SymbolSI value Equivalent values Units Speed of light c299792458 m s-1 29979245800299792.4581079252848.863241.07708426 cm s-1km s-1km hr-1AU yr-1 Planck’s constant…

Calculations for Kepler’s third law for a point-like mass and two comparable masses.

Calcluators for to-and-fro conversion of Celcius, Fahrehnhite, Rankine, and Kelvin temperature scales.

What is Newton-Kepler law of planetary motion? How is it different from the Kepler’s third law of planetary motion? And more.

This post discusses the usage of Kepler’s third law in case of our solar system. How it can be used to determine the semi-major axis given a planet’s time period and vice versa.

The famous Kepler’s law of planetary motion are discusses with mathematical derviations.

This post is the end result for the MaStar data processing. The parameters obtained through the given effective temperature, surface gravity, and the PSF magnitudes like mass, radius, luminosity, distance, flux etcetera are all discussed and visualized.

This post gives an overview of how telescopes gather data about celestial objects, how filter works, the SDSS ugriz filters, their conversion to UBVRI, color indices, how they can be determined and what do they have to do with temperature of stars.

This post discusses the methods of determining the distance to stars using the SDSS MaStar data magnitudes.

For g, r, and I filters for the PSF magnitudes provided the magnitudes were first converted to physical flux densities. The flux densities were then converted to flux, then the fluxes to radius using the flux-radius-luminosity relationship. After determining the distance, the apparent magnitudes were converted to absolute magnitudes of the star

Stellar magnitudes play an important role in classifying the stars. This post discusses both the apparent and absolute magnitudes of the star and the relationships from which these parameters can be obtained.