|
|
1.
|
|
|
Your names
|
| Context: |
|
NAME OF TRANSLATORS
|
|
|
|
|
To prevent privacy issues, this translation is not
available to anonymous users,
if you want to see it, please, log in
first. |
|
Translated and reviewed by
Launchpad Translations Administrators
|
| In upstream: |
|
Dwayne Bailey
|
|
|
Suggested by
Malcolm Hunter
|
|
Located in
rc.cpp:1362
|
|
|
2.
|
|
|
Your emails
|
| Context: |
|
EMAIL OF TRANSLATORS
|
|
|
|
|
To prevent privacy issues, this translation is not
available to anonymous users,
if you want to see it, please, log in
first. |
|
Translated and reviewed by
Launchpad Translations Administrators
|
| In upstream: |
|
dwayne@translate.org.za
|
|
|
Suggested by
Malcolm Hunter
|
|
Located in
rc.cpp:1363
|
|
|
4758.
|
|
|
<p> 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 zero. 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:</p> 
<li>Ra= 18:03:50.2 (J2000)</li>
<li>Dec = 30:0:16.8 (J2000)</li>
<p>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 ascension 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.</p>
<p>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</p>
<li>The heliocentric velocity (V<sub>hel</sub>) is computed by obtaining the scalar product of the radial velocity of the source referred to the LSR (V<sub>lsr</sub>) with the velocity of the Sun referred to the LSR (V<sub>sun</sub>:
<img src="vlsr1.png">
</li>
<li>The geocentric velocity (V<sub>geo</sub>) is obtained from the heliocentric velocity, the velocity of the Earth (V<sub>E</sub>) and its position for a given date and time:
<img src="vlsr2.png">
</li>
<li>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.</li> |
|
|
represents a line break.
Start a new line in the equivalent position in the translation.
|
|
|
|
|
<p> The Local Standard of Rest (LSR) is the location in which the mean value of the velocity of a selection of the stars in a solar neighbourhood is zero. 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:</p>
<li>Ra= 18:03:50.2 (J2000)</li>
<li>Dec = 30:0:16.8 (J2000)</li>
<p>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 ascension and declination. The radial velocity is usually obtained by analysing 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.</p>
<p>This calculator module allows to obtain the radial velocity of the source referred to the centre of the sun (what we call heliocentric velocity), referred to the centre of the Earth (geocentric velocity) and to the observer site (topocentric velocity) from the LSR radial velocity</p>
<li>The heliocentric velocity (V<sub>hel</sub>) is computed by obtaining the scalar product of the radial velocity of the source referred to the LSR (V<sub>lsr</sub>) with the velocity of the Sun referred to the LSR (V<sub>sun</sub>:
<img src="vlsr1.png">
</li>
<li>The geocentric velocity (V<sub>geo</sub>) is obtained from the heliocentric velocity, the velocity of the Earth (V<sub>E</sub>) and its position for a given date and time:
<img src="vlsr2.png">
</li>
<li>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.</li> |
|
Translated by
Benjamin Goodger
|
|
Reviewed by
Malcolm Hunter
|
| In upstream: |
|
<p> 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 zero. 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:</p>
<li>Ra= 18:03:50.2 (J2000)</li>
<li>Dec = 30:0:16.8 (J2000)</li>
<p>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 ascension 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.</p>
<p>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</p>
<li>The heliocentric velocity (V<sub>hel</sub>) is computed by obtaining the scalar product of the radial velocity of the source referred to the LSR (V<sub>lsr</sub>) with the velocity of the Sun referred to the LSR (V<sub>sun</sub>:
<img src="vlsr1.png">
</li>
<li>The geocentric velocity (V<sub>geo</sub>) is obtained from the heliocentric velocity, the velocity of the Earth (V<sub>E</sub>) and its position for a given date and time:
<img src="vlsr2.png">
</li>
<li>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.</li> |
|
|
Suggested by
Malcolm Hunter
|
|
|
|
|
5113.
|
|
|
Galactic Cooordinates
|
|
|
|
|
Galactic Coordinates
|
|
Translated and reviewed by
Benjamin Goodger
|
| In upstream: |
|
Galactic Cooordinates
|
|
|
Suggested by
Malcolm Hunter
|
|
|
|
|
5117.
|
|
|
<QT>Section with algorithms regarding information on solar system bodies coordinates and times<UL><LI><B>Planets Coordinates:</B> Coordinates for the planets, moon and sun at a given time and from a given position on Earth </LI></UL></QT>
|
|
|
|
|
<QT>Section with algorithms regarding information on solar system bodies' coordinates and times<UL><LI><B>Planets' Coordinates:</B> Coordinates for the planets, moon and sun at a given time and from a given position on Earth </LI></UL></QT>
|
|
Translated by
Benjamin Goodger
|
|
Reviewed by
Malcolm Hunter
|
| In upstream: |
|
<QT>Section with algorithms regarding information on solar system bodies coordinates and times<UL><LI><B>Planets Coordinates:</B> Coordinates for the planets, moon and sun at a given time and from a given position on Earth </LI></UL></QT>
|
|
|
Suggested by
Malcolm Hunter
|
|
|
|
Located in
tools/astrocalc.cpp:240
|
