Changelog¶
0.6.4¶
This release adds citation information to the documentation.
0.6.3¶
This release contains the source for the accepted JOSS paper describing pfsspy.
0.6.2¶
This release includes several small fixes in response to a review of pfsspy for the Journal of Open Source Software. Thanks to Matthieu Ancellin and Simon Birrer for their helpful feedback!
A permanent code of conduct file has been added to the repository.
Information on how to contribute to pfsspy has been added to the docs.
The example showing the performance of different magnetic field tracers has been fixed.
The docs are now clearer about optional dependencies that can increase performance.
The GONG example data has been updated due to updated data on the remote GONG server.
0.6.1¶
Bug fixes¶
Fixed some messages in errors raised by functions in
pfsspy.utils
.
0.6.0¶
New features¶
The
pfsspy.utils
module has been added, and contains various tools for loading and working with synoptic maps.pfsspy.Output
has a newbunit
property, which returns theUnit
of the input map.Added
pfsspy.Output.get_bvec()
, to sample the magnetic field solution at arbitrary coordinates.Added the
pfsspy.fieldline.FieldLine.b_along_fline
property, to sample the magnetic field along a traced field line.Added a guide to the numerical methods used by pfsspy.
Breaking changes¶
The
.al
property ofpfsspy.Output
is now private, as it is not intended for user access. If you really want to access it, use._al
(but this is now private API and there is no guarantee it will stay or return the same thing in the future).A
ValueError
is now raised if any of the input data topfsspy.Input
is non-finite or NaN. Previously the PFSS computation would run fine, but the output would consist entirely of NaNs.
Behaviour changes¶
The monopole term is now ignored in the PFSS calculation. Previously a non-zero (but small) monopole term would cause floating point precision issues, leading to a very noisy result. Now the monopole term is explicitly removed from the calculation. If your input has a non-zero mean value, pfsspy will issue a warning about this.
The data downloaded by the examples is now automatically downloaded and cached with
sunpy.data.manager
. This means the files used for running the examples will be downloaded and stored in yoursunpy
data directory if they are required.The observer coordinate information in GONG maps is now automatically set to the location of Earth at the time in the map header.
Bug fixes¶
The
date-obs
FITS keyword in GONG maps is now correctly populated.
0.5.3¶
Improved descriptions in the AIA overplotting example.
Fixed the ‘date-obs’ keyword in GONG metadata. Previously this just stored the date and not the time; now both the date and time are properly stored.
Drastically sped up the calculation of source surface and solar surface magnetic field footpoints.
0.5.2¶
Fixed a bug in the GONG synoptic map source where a map failed to load once it had already been loaded once.
0.5.1¶
Fixed some calculations in
pfsspy.carr_cea_wcs_header
, and clarified in the docstring that the input shape must be in[nlon, nlat]
order.Added validation to
pfsspy.Input
to check that the inputted map covers the whole solar surface.Removed ghost cells from
pfsspy.Output.bc
. This changes the shape of the returned arrays by one along some axes.Corrected the shape of
pfsspy.Output.bg
in the docstring.Added an example showing how to load ADAPT ensemble maps into a
CompositeMap
Sped up field line expansion factor calculations.
0.5.0¶
Changes to outputted maps¶
This release largely sees a transition to leveraging Sunpy Map objects. As such, the following changes have been made:
pfsspy.Input
now must take a sunpy.map.GenericMap
as an
input boundary condition (as opposed to a numpy array). To convert a numpy array
to a GenericMap
, the helper function
pfsspy.carr_cea_wcs_header
can be used:
map_date = datetime(...)
br = np.array(...)
header = pfsspy.carr_cea_wcs_header(map_date, br.shape)
m = sunpy.map.Map((br, header))
pfss_input = pfsspy.Input(m, ...)
pfsspy.Output.source_surface_br
now returns a GenericMap
instead of an array. To get the data array use source_surface_br.data
.
The new pfsspy.Output.source_surface_pils
returns the coordinates of
the polarity inversion lines on the source surface.
In favour of directly using the plotting functionality built into SunPy, the following plotting functionality has been removed:
pfsspy.Input.plot_input
. InsteadInput
has a newmap
property, which returns a SunPy map, which can easily be plotted usingsunpy.map.GenericMap.plot
.pfsspy.Output.plot_source_surface
. A map of \(B_{r}\) on the source surface can now be obtained usingpfsspy.Output.source_surface_br
, which again returns a SunPy map.pfsspy.Output.plot_pil
. The coordinates of the polarity inversion lines on the source surface can now be obtained usingpfsspy.Output.source_surface_pils
, which can then be plotted usingax.plot_coord(pil[0])
etc. See the examples section for an example.
Specifying tracing seeds¶
In order to make specifying seeds easier, they must now be a
SkyCoord
object. The coordinates are internally
transformed to the Carrington frame of the PFSS solution, and then traced.
This should make specifying coordinates easier, as lon/lat/r coordinates can be created using:
seeds = astropy.coordinates.SkyCoord(lon, lat, r, frame=output.coordinate_frame)
To convert from the old x, y, z array used for seeds, do:
r, lat, lon = pfsspy.coords.cart2sph
r = r * astropy.constants.R_sun
lat = (lat - np.pi / 2) * u.rad
lon = lon * u.rad
seeds = astropy.coordinates.SkyCoord(lon, lat, r, frame=output.coordinate_frame)
Note that the latitude must be in the range \([-\pi/2, \pi/2]\).
GONG and ADAPT map sources¶
pfsspy now comes with built in sunpy
map sources for GONG and ADAPT synoptic
maps, which automatically fix some non-compliant FITS header values. To use
these, just import pfsspy
and load the .FITS files as normal with sunpy.
Tracing seeds¶
pfsspy.tracing.Tracer
no longer has a transform_seeds
helper method, which
has been replaced by coords_to_xyz
and
pfsspy.tracing.Tracer.xyz_to_coords
. These new methods convert
between SkyCoord
objects, and Cartesian xyz coordinates
of the internal magnetic field grid.
0.4.3¶
Improved the error thrown when trying to use :class`pfsspy.tracing.FotranTracer` without the
streamtracer
module installed.Fixed some layout issues in the documentation.
0.4.2¶
Fix a bug where :class`pfsspy.tracing.FotranTracer` would overwrite the magnetic field values in an
Output
each time it was used.
0.4.1¶
Reduced the default step size for the
FortranTracer
from 0.1 to 0.01 to give more resolved field lines by default.
0.4.0¶
New fortran field line tracer¶
pfsspy.tracing
contains a new tracer,
FortranTracer
. This requires and uses the
streamtracer package
which does streamline tracing rapidly in python-wrapped
fortran code. For large numbers of field lines this results in an ~50x
speedup compared to the PythonTracer
.
Changing existing code to use the new tracer is as easy as swapping out
tracer = pfsspy.tracer.PythonTracer()
for
tracer = pfsspy.tracer.FortranTracer()
. If you notice any issues with the
new tracer, please report them at https://github.com/dstansby/pfsspy/issues.
Changes to field line objects¶
pfsspy.FieldLines
andpfsspy.FieldLine
have moved topfsspy.fieldline.FieldLines
andpfsspy.fieldline.FieldLine
.FieldLines
no longer hassource_surface_feet
andsolar_feet
properties. Instead these have moved to the newpfsspy.fieldline.OpenFieldLines
class. All the open field lines can be accessed from aFieldLines
instance using the newopen_field_lines
property.
Changes to Output
¶
pfsspy.Output.bg
is now returned as a 4D array instead of three 3D arrays. The final index now indexes the vector components; see the docstring for more information.
0.3.2¶
Fixed a bug in
pfsspy.FieldLine.is_open
, where some open field lines were incorrectly calculated to be closed.
0.3.1¶
Fixed a bug that incorrectly set closed line field polarities to -1 or 1 (instead of the correct value of zero).
FieldLine.footpoints
has been removed in favour of the newpfsspy.FieldLine.solar_footpoint
andpfsspy.FieldLine.source_surface_footpoint
. These each return a single footpoint. For a closed field line, see the API docs for further details on this.pfsspy.FieldLines
has been added, as a convenience class to store a collection of field lines. This means convenience attributes such aspfsspy.FieldLines.source_surface_feet
can be used, and their values are cached greatly speeding up repeated use.
0.3.0¶
The API for doing magnetic field tracing has changed. The new
pfsspy.tracing
module containsTracer
classes that are used to perform the tracing. Code needs to be changed from:fline = output.trace(x0)
to:
tracer = pfsspy.tracing.PythonTracer() tracer.trace(x0, output) flines = tracer.xs
Additionally
x0
can be a 2D array that contains multiple seed points to trace, taking advantage of the parallelism of some solvers.The
pfsspy.FieldLine
class no longer inherits fromSkyCoord
, but theSkyCoord
coordinates are now stored inpfsspy.FieldLine.coords
attribute.pfsspy.FieldLine.expansion_factor
now returnsnp.nan
instead ofNone
if the field line is closed.pfsspy.FieldLine
now has a~pfsspy.FieldLine.footpoints
attribute that returns the footpoint(s) of the field line.
0.2.0¶
pfsspy.Input
andpfsspy.Output
now take the optional keyword argument dtime, which stores the datetime on which the magnetic field measurements were made. This is then propagated to the obstime attribute of computed field lines, allowing them to be transformed in to coordinate systems other than Carrington frames.pfsspy.FieldLine
no longer overrrides the SkyCoord__init__
; this should not matter to users, as FieldLine objects are constructed internally by callingpfsspy.Output.trace
0.1.5¶
Output.plot_source_surface
now accepts keyword arguments that are given to Matplotlib to control the plotting of the source surface.
0.1.4¶
Added more explanatory comments to the examples
Corrected the dipole solution calculation
Added
pfsspy.coords.sph2cart
to transform from spherical to cartesian coordinates.
0.1.3¶
pfsspy.Output.plot_pil
now accepts keyword arguments that are given to Matplotlib to control the style of the contour.pfsspy.FieldLine.expansion_factor
is now cached, and is only calculated once if accessed multiple times.