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List:       kde-commits
Subject:    kdeedu/kstars/kstars/tools
From:       Pablo de Vicente <p.devicente () wanadoo ! es>
Date:       2005-04-10 16:43:17
Message-ID: 20050410164317.7BDB4495 () office ! kde ! org
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CVS commit by pvicente: 

Polished the text, but yet unfinished. Need more time for that.


  M +4 -5      modcalcvlsrdlg.ui   1.3


--- kdeedu/kstars/kstars/tools/modcalcvlsrdlg.ui  #1.2:1.3
@@ -981,10 +981,9 @@
                         </property>
                         <property name="text">
-                            <string>&lt;p&gt; The Local Standard of Rest (LSR) is \
the centroid of motion of the local group of stars in the neighborhood of the Sun. \
There are several coordinates for the solar apex. Here we use the radioastronomical \
position:&lt;/p&gt; +                            <string>&lt;p&gt; The Local Standard \
of Rest (LSR) is the location in which the mean value of the velocity of a selection \
of the stars in solar neighboorhood is cero. The local solar motion, that is, the \
velocity of the sun referred to the Local Standard of Rest is not null: the sun moves \
with a velocity of 20 km/s towards a point called, solar apex, whose coordinates \
are:&lt;/p&gt;  &lt;li&gt;Ra= 18:03:50.2 (J2000)&lt;/li&gt;
 &lt;li&gt;Dec = 30:0:16.8 (J2000)&lt;/li&gt;
-&lt;p&gt;The Sun moves away from this location with a velocity of 20.0 \
                km/s.&lt;/p&gt;
-&lt;p&gt;Astronomical sources move relative to the Sun and their velocity can be \
decomposed in radial velocity, and velocity on the plane of the sky; also know as \
proper motion. The radial velocity is usually obtained by analyzing their spectral \
emission and the frequency shift of the lines due to Doppler effect. Observational \
                astronomers usually refer the radial to the LSR.&lt;/p&gt;
-&lt;p&gt;This calculator module allows you to obtain the radial velocity of the \
source referred to the center of the sun (heliocentric velocity), referred to the \
center of the Earth (geocentric velocity) and to the observer site (topocentric \
velocity) from the LSR radial velocity&lt;/p&gt; +&lt;p&gt;Astronomical sources move \
relative to the Sun and their velocity can be decomposed in radial velocity, and \
velocity on the plane of the sky, also know as proper motion in right ascention and \
declination. The radial velocity is usually obtained by analyzing their spectral \
emission and the frequency shift of the lines due to Doppler effect. Observational \
astronomers usually refer source's radial velocity to the LSR.&lt;/p&gt; \
+&lt;p&gt;This calculator module allows to obtain the radial velocity of the source \
referred to the center of the sun (what we call heliocentric velocity), referred to \
the center of the Earth (geocentric velocity) and to the observer site (topocentric \
velocity) from the LSR radial velocity&lt;/p&gt;  &lt;li&gt;The heliocentric velocity \
(V&lt;sub&gt;hel&lt;/sub&gt;) is computed by obtaining the scalar product of the \
radial velocity of the source referred to the LSR (V&lt;sub&gt;lsr&lt;/sub&gt;) with \
the velocity of the Sun referred to the LSR (V&lt;sub&gt;sun&lt;/sub&gt;:  &lt;img \
src="vlsr1.png"&gt; @@ -993,5 +992,5 @@
 &lt;img src="vlsr2.png"&gt;
 &lt;/li&gt;
-&lt;li&gt;The topocentric velocity is obtained from the geocentric velocity, the \
position on the Earth, and the date and time at which we want to determine the radial \
velocity of the source.&lt;/li&gt;</string> +&lt;li&gt;The topocentric velocity is \
obtained from the  geocentric velocity, the position on the Earth, and the date and \
time at which we desire to know the radial velocity of the \
source.&lt;/li&gt;</string>  </property>
                     </widget>


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