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Project Description

Overview

The purpose of this project is to estimate physical quantities of an eclipsing, spectroscopic binary star system using observed quantities from photometry and spectroscopy. The estimated physical quantities serve as input to a more complete numerical model such as that of Wilson-Devinney, c.f. chapter 7 of [1]. The model used in this project is a simple, spherical detached binary star model with no orbital eccentricity and no limb darkening. The model is from chapter 7 of [2] and chapter 7 of [3].

Input observed quantities

  • Relative times of begin/end ingress/egress and mid-eclipse.
  • Orbital period.
  • Light levels during occultation (primary eclipse), transit (secondary eclipse), and outside of eclipse.
  • Stellar radial velocities.

Output estimated physical quantities

  • Orbital inclination angle.
  • Orbital radii.
  • Stellar masses.
  • Stellar radii.
  • Ratio of stellar radiative fluxes.
  • Ratio of stellar effective temperatures.
  • Ratio of stellar luminosites.

Examples and Q&A forum

Citations

Recent changes

  • [v0.1.3] - 20150420T180000
    • Created Google group, DOI for citations, CHANGELOG.rst, IPython Notebook examples.
    • Fixed special cases where solver for inclination did not converge.
  • [v0.1.2] - 20150123T172000
    • Initial release to PyPI.
Release History

Release History

0.1.3

This version

History Node

TODO: Figure out how to actually get changelog content.

Changelog content for this version goes here.

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0.1.2

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Changelog content for this version goes here.

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0.1.1

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TODO: Figure out how to actually get changelog content.

Changelog content for this version goes here.

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Download Files

Download Files

TODO: Brief introduction on what you do with files - including link to relevant help section.

File Name & Checksum SHA256 Checksum Help Version File Type Upload Date
binstarsolver-0.1.3.tar.gz (21.5 kB) Copy SHA256 Checksum SHA256 Source Apr 20, 2015

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