A brief tour of sunpy¶
This brief tutorial will walk you through some of the functionality offered by the sunpy core package. Start by reading this tutorial and trying out some of the examples demonstrated. Once you’ve completed the tutorial check out the rest of the User Guide for a more thorough look at the functionality available.
This tour makes use of a number of sample data files that will need to be downloaded.
This downloading will happen automatically when using the module
Maps are the primary data type in sunpy. They are spatially aware data arrays. There are maps for a 2D image, a time series of 2D images or temporally aligned 2D images.
Creating a Map
sunpy supports many different data products from various sources ‘out of the
box’. We shall use SDO’s AIA instrument as an example in this tutorial. The
general way to create a Map from one of the supported data products is with the
Map function from the
Map takes either a filename, a list of
filenames or a data array and header. We can test
import sunpy.data.sample import sunpy.map aia = sunpy.map.Map(sunpy.data.sample.AIA_171_IMAGE) aia.peek()
This returns a map named
aia which can be manipulated with standard sunpy map commands.
For more information about maps checkout the map guide
and the Maps (sunpy.map).
sunpy handles time series data, fundamental to the study of any real world phenomenon, by creating a TimeSeries object. A timeseries consists of two parts; times and measurements taken at those times. The data can either be in your current Python session, alternatively within a local or remote file. In the code block that follows, data is taken from a file containing samples from a file containing samples from the GOES satellite’s X-ray Sensors (XRS).
import numpy as np import sunpy.data.sample import sunpy.timeseries as ts my_timeseries = ts.TimeSeries(sunpy.data.sample.GOES_XRS_TIMESERIES, source='XRS') my_timeseries.peek()
We’ve created this timeseries object by passing TimeSeries a string which
represents the name of a GOES lightcurve file. The
.peek() method plots the timeseries
data and displays the plot with some default settings. You can also use
my_timeseries.plot() if you want more
control over the style of the output plot.
For more information about TimeSeries, check out the timeseries guide and the and the Timeseries (sunpy.timeseries).
sunpy uses a matplotlib-like interface to its plotting so more complex plots can be built by combining sunpy with matplotlib. If you’re not familiar with plotting in matplotlib, you should learn the basics before continuing with this guide.
Let’s begin by creating a simple plot of an AIA image. To make things easy,
sunpy includes several example files which are used throughout the docs. These
files have names like
Try typing the below example into your interactive Python shell.
import sunpy.map import sunpy.data.sample aia = sunpy.map.Map(sunpy.data.sample.AIA_171_IMAGE) aia.peek()
If everything has been configured properly you should see an AIA image with the default AIA 17.1 colormap, a colorbar on the right-hand side and a title and some labels.
There is lot going on here, but we will walk you through the example. Briefly,
the first line is importing sunpy, and the second importing the sample data
files. On the third line we create a sunpy Map object which is a spatially-aware
image. On the last line we then plot the
Map object, using the built in ‘quick plot’
sunpy uses a matplotlib-like interface to it’s plotting so more complex plots can be built by combining sunpy with matplotlib.
import sunpy.map import matplotlib.pyplot as plt import sunpy.data.sample aia = sunpy.map.Map(sunpy.data.sample.AIA_171_IMAGE) fig = plt.figure() ax = plt.subplot(111, projection=aia) aia.plot() aia.draw_limb() aia.draw_grid() plt.colorbar() plt.show()
For more information check out Plotting in sunpy.
Solar Physical Constants¶
sunpy contains a convenient list of solar-related physical constants. Here is a short bit of code to get you started:
>>> from sunpy.sun import constants as con # one astronomical unit (the average distance between the Sun and Earth) >>> print(con.au) Name = Astronomical Unit Value = 149597870700.0 Uncertainty = 0.0 Unit = m Reference = IAU 2012 Resolution B2 # the solar radius >>> print(con.radius) Name = Nominal solar radius Value = 695700000.0 Uncertainty = 0.0 Unit = m Reference = IAU 2015 Resolution B 3
Not all constants have a shortcut assigned to them (as above). The rest of the constants are stored in a dictionary. The following code grabs the dictionary and gets all of the keys.:
>>> solar_constants = con.constants >>> solar_constants.keys() dict_keys(['mass', 'radius', 'luminosity', 'mean distance', 'perihelion distance', 'aphelion distance', 'age', 'solar flux unit', 'visual magnitude', 'average angular size', 'surface area', 'average density', 'surface gravity', 'moment of inertia', 'volume', 'escape velocity', 'oblateness', 'metallicity', 'sunspot cycle', 'average intensity', 'effective temperature', 'mass conversion rate', 'center density', 'center temperature', 'absolute magnitude', 'mean energy production', 'ellipticity', 'GM', 'W_0', 'sidereal rotation rate', 'first Carrington rotation (JD TT)', 'mean synodic period', 'alpha_0', 'delta_0'])
You can also use the function
sunpy.sun.constants.print_all() to print out a table of all of the values
available. These constants are provided as a convenience so that everyone is using the same
(accepted) values. For more information check out Solar properties (sunpy.sun).
Quantities and Units¶
Many capabilities in sunpy make use of physical quantities that are specified
with units. sunpy uses
units to implement this functionality.
Quantities and units are powerful tools for keeping track of variables with
physical meaning and make it straightforward to convert the same physical
quantity into different units. To learn more about the capabilities of
quantities and units, consult Units or
the astropy tutorial.
To demonstrate this, let’s look at the solar radius constant. This is a physical quantity that can be expressed in length units
>>> from sunpy.sun import constants as con >>> con.radius <<class 'astropy.constants.iau2015.IAU2015'> name='Nominal solar radius' value=695700000.0 uncertainty=0.0 unit='m' reference='IAU 2015 Resolution B 3'>
shows the solar radius in units of meters. The same physical quantity can be expressed in different units instead using the
>>> con.radius.to('km') <Quantity 695700. km>
>>> import astropy.units as u >>> con.radius.to(u.km) <Quantity 695700. km>
If, as is sometimes the case, you need just the raw value or the unit from a quantity, you can access these individually
`unit attributes, respectively:
>>> r = con.radius.to(u.km) >>> r.value 695700.0 >>> r.unit Unit("km")
This is useful, but the real power of units is in using them in calculations. Suppose you have the radius of a circle and would like to calculate its area. The following code implements this:
>>> import numpy as np >>> import astropy.units as u >>> def circle_area(radius): ... return np.pi * radius ** 2
The first line imports numpy, and the second line imports astropy’s units module. The function then calculates the area based on a given radius. When it does this, it tracks the units of the input and propagates them through the calculation. Therefore, if we define the radius in meters, the area will be in meters squared:
>>> circle_area(4 * u.m) <Quantity 50.26548246 m2>
This also works with different units, for example
>>> from astropy.units import imperial >>> circle_area(4 * imperial.foot) <Quantity 50.26548246 ft2>
As demonstrated above, we can convert between different systems of measurement. For example, if you want the area of a circle in square feet, but were given the radius in meters, then you can convert it before passing it into the function:
>>> circle_area((4 * u.m).to(imperial.foot)) <Quantity 541.05315022 ft2>
or you can convert the output:
>>> circle_area(4 * u.m).to(imperial.foot ** 2) <Quantity 541.05315022 ft2>
This is an extremely brief summary of the powerful capbilities of Astropy units. To find out more, see the the astropy tutorial and documentation
Working with Times¶
sunpy also contains a number of convenience functions for working with dates and times. Here is a short example:
>>> import sunpy.time # parsing a standard time strings >>> sunpy.time.parse_time('2004/02/05 12:00') <Time object: scale='utc' format='isot' value=2004-02-05T12:00:00.000> # This returns a astropy.time.Time object. All sunpy functions which require # time as an input sanitize the input using parse_time. # the julian day >>> sunpy.time.parse_time((2010,4,30)).jd 2455316.5 # TimeRange objects are useful for representing ranges of time >>> time_range = sunpy.time.TimeRange('2010/03/04 00:10', '2010/03/04 00:20') >>> time_range.center <Time object: scale='utc' format='isot' value=2010-03-04T00:15:00.000>
For more information about working with time in sunpy checkout the time guide.
sunpy supports searching for and fetching data from a variety of sources,
including the VSO and the
JSOC. The majority of sunpy’s clients can be
queried using the
sunpy.net.Fido interface. An example of searching the VSO using this
>>> from sunpy.net import Fido, attrs as a >>> results = Fido.search(a.Time("2011-09-20T01:00:00", "2011-09-20T02:00:00"), ... a.Instrument.eit) >>> Fido.fetch(results, path="./directory/") ['./directory/efz20110920.010015', './directory/efz20110920.010613', './directory/efz20110920.011353', './directory/efz20110920.011947']
For more information and examples of downloading data with sunpy see Acquiring Data.
The database package can be used to keep a local record of all files downloaded from the VSO, this means that two searches of the VSO which overlap will not re-download data.
A simple example of this is shown below:
>>> import astropy.units as u >>> from sunpy.net import Fido, attrs as a >>> from sunpy.database import Database >>> db = Database() >>> db.fetch(a.Time("2011-09-20T01:00:00", "2011-09-20T02:00:00"), ... a.Instrument.aia, a.Sample(45*u.min)) >>> db.commit() >>> db <Table length=4> id observation_time_start observation_time_end ... download_time size str1 str19 str19 ... str19 str7 ---- ---------------------- -------------------- ... ------------------- ------- 1 2011-09-20 01:00:00 2011-09-20 01:00:01 ... 2020-11-21 14:15:30 66200.0 2 2011-09-20 01:00:00 2011-09-20 01:00:01 ... 2020-11-21 14:15:30 66200.0 3 2011-09-20 01:45:00 2011-09-20 01:45:01 ... 2020-11-21 14:15:30 66200.0 4 2011-09-20 01:45:00 2011-09-20 01:45:01 ... 2020-11-21 14:15:30 66200.0
If you then do a second query:
>>> db.fetch(a.Time("2011-09-20T01:00:00", "2011-09-20T02:45:00"), ... a.Instrument.aia, a.Sample(45*u.min)) >>> db.commit() >>> db <Table length=6> id observation_time_start observation_time_end ... download_time size str1 str19 str19 ... str19 str7 ---- ---------------------- -------------------- ... ------------------- ------- 1 2011-09-20 01:00:00 2011-09-20 01:00:01 ... 2020-11-21 14:15:30 66200.0 2 2011-09-20 01:00:00 2011-09-20 01:00:01 ... 2020-11-21 14:15:30 66200.0 3 2011-09-20 01:45:00 2011-09-20 01:45:01 ... 2020-11-21 14:15:30 66200.0 4 2011-09-20 01:45:00 2011-09-20 01:45:01 ... 2020-11-21 14:15:30 66200.0 5 2011-09-20 02:30:00 2011-09-20 02:30:01 ... 2020-11-21 14:17:51 66200.0 6 2011-09-20 02:30:00 2011-09-20 02:30:01 ... 2020-11-21 14:17:51 66200.
A query can then be performed against the database to get the records:
>>> entries = db.search(a.Time("2011-09-20T01:45:00", "2011-09-20T02:15:00"), a.Instrument.aia) >>> len(entries) 4
You can see that only two extra records were added to the database. For more information check out the Using the database package.