p-winds v2.0.1 beta

This is the beta version of p-winds version 2.0.1. The main changes in this version are:

• The addition of new functions in the hydrogen and lines modules that include the capability to model transmission spectra in the Balmer-series lines of hydrogen. This implementation is based on the formulation laid out in Wyttenbach et al. (2020). Thanks to @jseideleso for contributing to this!
• Other small improvements and bug corrections.

p-winds v1.4.7

This is an important update to p-winds that corrects bugs and implement a cool new algorithm that has been requested in the past. Updating to this version is highly recommended.

Change log:

• Corrected a bug in the calculation of the Gaussian width of Voigt profiles in the transit module.
• Added the option to pass gas_temperature as an array (in function of radius from planet) instead of only a float or int. This is useful if you have a model with self-consistently calculated temperatures and do not need to assume an isothermal profile.
• Other small improvements to documentation and code reading.

p-winds v2.0 beta

This is the beta release of p-winds version 2.0. The newest addition is the brand new module fluid, which calculates self-consistent hydrodynamic simulations instead of assuming an isothermal Parker wind model. This version contains a wrapper for the ATES code, originally developed by Andrea Caldiroli. Please follow the installation instructions and documentation for details on how to use the new module.

Change log:

• Implemented the new module fluid, which contains a wrapper for the hydrodynamic escape code ATES
• General improvements in code comments and documentation

p-winds v1.4.6

This is a fairly small, but useful update to p-winds. We added a new function in the tools module that generates a "generic" standard spectrum (standard_spectrum()) based on the stellar type and semi-major axis. The available stellar types are:

• 'mid-A' (based on HR 8799)
• 'early-F' (based on WASP-17)
• 'late-F' (based on HD 108147)
• 'early-G' (based on HD 149026)
• 'solar' (based on the Sun)
• 'young-sun' (based on iota Horologii)
• 'late-G' (based on TOI-193)
• 'active-K' (based on epsilon Eridanii)
• 'early-K' (based on HD 97658)
• 'late-k' (based on WASP-43)
• 'active-M' (based on Proxima Centauri)
• 'early-M' (based on GJ 436)
• 'late-M' (based on TRAPPIST-1)

Another important change: the environment variable that defines the location of the MUSCLES spectra is now $PWINDS_REFSPEC_DIR. Please modify your workflow accordingly.

If you use any of these, please cite the papers that produced the spectra.
Enjoy it!

p-winds version 1.4.5

Version 1.4.5 of p-winds improves documentation and changes the way that MUSCLES spectra are handled. Here is the changelog:

• Added almost all MUSCLES, Mega-MUSCLES and MUSCLES Extension stellar spectra are now supported in tools.generate_muscles_spectrum() function. See the documentation for details.
• Since there are many more spectra, starting on this version the MUSCLES fits files are not included in the p-winds package. Now the user needs to manually download them (either from the survey website or from this convenience Box link), and then set a $MUSCLES_DIR environment variable pointing to the location of the fits files. See installation instructions.
• General bug fixes.

p-winds v1.4.4

Version 1.4.4 of p-winds calculates the density profiles of exospheric metals! Here is the changelog:

• New module: carbon.py is used to calculate the distribution of neutral, singly-ionized and doubly-ionized carbon in an exoplanet's upper atmosphere.
• New module: oxygen.py is used to calculate the distribution of neutral and singly-ionized oxygen in an exoplanet's upper atmosphere.
• New module: lines.py stores spectral line information. This information was previously stored in microphysics.py, but was moved to avoid bloating the latter module. Please pay attention to this new usage of microphysics.py! As always, check the documentation to learn more.
• helium.py now includes a function ion_fraction() that calculates the ion fraction of helium more quickly than the population_fraction() function.
• The function make_spectrum_from_file() now has an option to scale an input spectrum by systemic distance and the semi-major axis of a planet around it.
• New examples in the documentation: Roche lobe effects and exospheric metals.
• General bug fixes and updates to docstrings.

A paper describing the carbon and oxygen modules is being submitted for refereed publication soon. As always, please check the documentation of the code for guidance on the functions parameters!

p-winds v1.3.4

This is a patch to the stable version of p-winds. Here are the changes:

• Corrected a bug in hydrogen.py where the code passed velocity and radii to parker.average_molecular_weight() in units of values at the sonic radius instead of km/s and Jupiter radii. This correction has only a small impact to the resulting models.
• Improved rendering of the documentation in ReadTheDocs.
• Some small updates in the test suites.

p-winds v1.3.3

This patch corrects several small bugs in the code (see issue #36).

p-winds v1.3.2

This patch contains several optimizations for p-winds and some new features. We highly recommend users to update. Changelog:

• Small optimization in parker.py when running structure() and structure_tidal()
• Added options to return reaction rates in hydrogen.py and helium.py when calculating the H ion fraction or He population fraction. See an example in the documentation (more specifically the Quickstart notebook).
• Added a function to return the He ion fraction in helium.py (does not calculate the singlet/triplet He atoms)
• Removed an annoying warning that could appear when using MUSCLES spectra generated from tools.py
• Some functions that were previously implemented in microphysics.py were moved to lines.py. See the documentation to learn how this affects your own codes.
• Significant optimization on helium.population_fraction() that cuts down computation of He profiles by a factor of ~50% and improves numerical stability of the solution.
• Added an option to manually set the grid resolution of the line-of-sight direction when using transit.radiative_transfer_2d() with the parameter z_grid_size. Grids with lower resolution than the standard on in the code will accelerate the computation of the 'formal' absorption profiles. It does not affect the 'average' method.

p-winds v1.3.1

This is a patch that corrects a critical bug in p-winds 1.3. In previous versions, there was an error in the calculation of density_r in structure_tidal() that yielded strange, but still reasonable results. The calculation in question is that of Eq. D10 in Vissapragada et al. (2022). The mistake was in the implementation of the second term of this equation. It has been corrected in this patch, version 1.3.1.

Please update your code to match this correction.