- Overview of Euler
- Download some astronomical functions
- Using the astronomical functions
- Adding your own functions

Euler is an interactive 'expression evaluator' that operates in a Notepad style window under Windows 95 and other Microsoft 32 bit operating systems, as well as Unix. Euler is written and actively maintained by Dr Rene Grothmann.

I have contributed a simple 'package' of basic astronomical functions for use with Euler. This package provides functions to calculate apparent positions of the Moon, Sun and major planets using routines of 5 to 10 arcsecond accuracy and simple corrections for nutation and aberration, as well as calculating topocentric positions and the altitude and azimuth. Physical ephermerides for the Moon and major planets will be added in the future, as will rising and setting phenomena.

Euler is obtained as a ZIP file from the following Web
site

**
http://mathsrv.ku-eichstaett.de/MGF/homes/grothmann/euler/euler.html
**

When you expand the ZIP file, there is a folder called Docs
that contains Dr Grothmann's documentation for Euler. I would
suggest you work through the *Introduction*,
*Basics* and *Expressions and Matrices* sections
before using the astronomical functions.

I have hacked together some astronomical functions from books
by Meeus, Duffett-Smith and
Montenbruck and Pfleger. These functions are
collected togther in a Euler 'program file' called
`astro.e`.

To make these functions available to Euler, you should

- Save the file
`astro.e`to your hard drive - Copy or move this file to the
`progs`folder within the Euler folder - Start Euler and type '
`load astro`' at the command prompt within Euler - You should see the '
`astronomical functions`' message appear in Euler. There will also be a date in this message - check this page for later versions of`astro.e`.

You can edit the configuration file `euler.cfg` so
that `astro.e` loads each time you start Euler - see the Euler
manual for details.

The best way to illustrate the use of the `astro.e`
functions is to describe a typical interactive session. In this
session we will:-

- load the '
`astro.e`' package into Euler - list the functions available
- get help with the '
`tmoon`' function - define a variable '
`now`' that holds the current TD date in days since J2000.0 - Find the apparent equatorial coordinates of the Sun on that
date, and store the position in a variable called '
`psun`' - Find the apparent (geocentric) coordinates of the Moon on
that date, and store in a variable called '
`gmoon`' - Define a vector variable called '
`here`' that holds the longitude, latitude, height above sea level, temperature and pressure at our observing location - Find the apparent
*topocentric*position of the Moon, and store the position in a variable called '`pmoon`' - Compare the topocentic and geocentric positions of the Moon
- Compare the position of the Sun and the (topocentric) Moon
- Calculate the altitude and azimuth of the Sun and the Moon and store the positions in suitable variables
- Recalculate everything for a slightly different time

The transcript of the session is reproduced below. You type
commands after the prompt '`>`', and the response
appears on the next line indented by about 4 spaces. Equatorial
coordinates are returned in a vector consisting of the RA in
*degrees*, the declination in degrees, and the distance of
the object in either a.u. (or in Km for the Moon).

>load astro ----------------------------------------------------- Astronomical functions 1999-08-18 Type 'help astro(RETURN)' for list of functions ----------------------------------------------------- >help astro function astro () ## Astronomical functions taken from ## Jean Meeus - 'Astronomical Algorithms' ## Montenbruck and Pfleger - 'Astronomy on the Personal Computer' ## Duffett-Smith - 'Practical astronomy with your calculator' ## other sources. ## For information on a function named fred, type 'help fred'. ## ## day jday gst nutation ## hmercury hvenus hearth hmars hjupiter ## mercury venus sun mars jupiter ## gmer gven gmar gjup ## gmoon amoon moon tmoon ## equatorial apparent mean altaz raltaz ## cart sph ## table ## ddegrees dsin dcos dtan dasin dacos datan datan2 ## brum reekie settle ## >help tmoon function tmoon (day,station) ## returns: topcentric equatorial coordinates of Moon ## given: TD instant in 'day' ## 'station' - vector lat, long, height (m), temp (C), ## and pressure (mB) of observing location >now = day(1999, 8, 11, 10, 17) -143.072 >psun = sun(now) 140.754 15.3374 1.01358 >gmoon = moon(now) 140.429 15.9114 373195 >here = [-1.9167, 52.5, 120, 17, 1011 ] -1.9167 52.5 120 17 1011 >pmoon = tmoon(now, here) 140.729 15.3036 368556 >pmoon - gmoon 0.300715 -0.60774 -4639.18 >psun - pmoon 0.0243673 0.0337465 -368555 >sunbrum = altaz(now, here, psun) 137.411 46.3381 1.01358 >moonbrum = altaz(now, here, pmoon) 137.463 46.3176 368556 >sunbrum-moonbrum -0.0516406 0.0204827 -368555 >

To recalculate all the quantities for a different time, just

- scroll up to the
`day`function - alter the time - say change the hour from 10 to 11
- press return - the value for days should change, and the cursor will jump to the next command line
- press return to recalculate the next command - the values will change as the function re-calculates
- press return on each command until they have all re- calculated

Note that Euler will not automatically recalculate when the value of variables defined earlier is changed - you have to press return each time to force recalculation.

This ability to set up a series of commands and then change parameters and recalculate new answers makes 'trial and error' calculations for astronomical configurations possible. The next logical move is to combine the calculation sequence into a function in its own right.

Functions can be defined at the Euler prompt and saved in
'notepad' files for re-use. You can also write functions with an
ordinary text editor and save collections of functions as
'programs' with the file extension `.e`. See the Euler
manual for syntax, examples and details.

You can just add the code for your astronomical functions to
`astro.e` - if you crack moonrise and set from any
latitude, I'd like a copy!

Below is the code for the `day` function that converts
from a date in UT (strictly dynamical time) to the number of days
since J2000.

function day(y, m, d, h, min) ## returns the days since J2000.0 number assuming the Gregorian calendar ## after 1582 Oct 4th given the year, month, day, hour and minute ## This method is modified from Duffett-Smith Calculator page 7 ## Negative years CE are numbered according to the astronomical ## convention - i.e. calendrical year 1 BC is year zero in this function greg = y*10000 + m*100 + d; if m == 1 || m == 2; y = y - 1; m = m + 12; endif; if greg > 15821004; a = floor(y/100); b = 2 - a + floor(a/4); else; b = 0; endif; c = floor(365.25 * y); d1 = floor(30.6001 * (m + 1)); return b + c + d1 -730550.5 + d + (h+min/60)/24; endfunction

As you can see, the overall format of the function is similar
to a function in `QBASIC` or most other languages. The
boolean operators for use in 'if' statements are similar to those
of C. If you omit a semicolon at the end of each line, the value
of that line will be echoed to the Euler window when the function
is called.

[ Root ]

Last Modified 18th August 1999

Keith Burnett