[RFR] po://kstars-doc/fr/kstars_flux.po

[steve]

Merci pour vos relectures.
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# translation of kstars_flux.po to français
# traduction de kstars_flux.po en Français
#
# Delafond <gerard at delafond.org>, 2003.
# Ludovic Grossard <grossard at kde.org>, 2004, 2012.
# Stanislas Zeller <uncensored.assault at gmail.com>, 2008.
# steve <stax at ik.me>, 2022.
msgid ""
msgstr ""
"Project-Id-Version: kstars_flux_3.5.8\n"
"Report-Msgid-Bugs-To: https://bugs.kde.org\n"
"POT-Creation-Date: 2021-03-28 16:23+0000\n"
"PO-Revision-Date: 2022-06-11 07:31+0200\n"
"Last-Translator: steve <stax at ik.me>\n"
"Language-Team: French <kde-francophone at kde.org>\n"
"Language: fr\n"
"MIME-Version: 1.0\n"
"Content-Type: text/plain; charset=UTF-8\n"
"Content-Transfer-Encoding: 8bit\n"
"Plural-Forms: nplurals=2; plural=(n > 1);\n"

#. Tag: author
#. +> trunk5
#: flux.docbook:5
#, no-c-format
msgid "<firstname>Jasem</firstname> <surname>Mutlaq</surname>"
msgstr "<firstname>Jasem</firstname> <surname>Mutlaq</surname>"

#. Tag: title
#. +> trunk5
#: flux.docbook:13
#, no-c-format
msgid "<title>Flux</title>"
msgstr "<title>Flux</title>"

#. Tag: primary
#. +> trunk5
#: flux.docbook:14
#, no-c-format
msgid "<primary>Flux</primary>"
msgstr "<primary>Flux</primary>"

#. Tag: seealso
#. +> trunk5
#: flux.docbook:15
#, no-c-format
msgid "Luminosity"
msgstr "Luminosité"

#. Tag: para
#. +> trunk5
#: flux.docbook:18
#, no-c-format
msgid ""
"The <firstterm>flux</firstterm> is the amount of energy that passes through "
"a unit area each second."
msgstr ""
"Le <firstterm>flux</firstterm> est la quantité d'énergie qui passe par une "
"unité de surface chaque seconde."

#. Tag: para
#. +> trunk5
#: flux.docbook:22
#, no-c-format
msgid ""
"Astronomers use flux to denote the apparent brightness of a celestial body. "
"The apparent brightness is defined as the amount of light received from a "
"star above the earth atmosphere passing through a unit area each second. "
"Therefore, the apparent brightness is simply the flux we receive from a "
"star."
msgstr ""
"Les astronomes utilisent le flux pour dénoter la luminosité apparente d'un "
"corps céleste. La luminosité apparente est définie comme la quantité de "
"lumière reçue d'une étoile au-dessus de l'atmosphère terrestre passant par "
"une unité de surface chaque seconde. Par conséquent, la luminosité apparente"
" est simplement le flux que nous recevons d'une étoile."

#. Tag: para
#. +> trunk5
# unreviewed-context
#: flux.docbook:27
#, no-c-format
msgid ""
"The flux measures the <emphasis>rate of flow</emphasis> of energy that "
"passes through each cm<superscript>2</superscript> (or any unit area) of an "
"object's surface each second. The detected flux depends on the distance from"
" the source that radiates the energy. This is because the energy has to "
"spread over a volume of space before it reaches us. Let us assume that we "
"have an imaginary balloon that encloses a star. Each dot on the balloon "
"represents a unit of energy emitted from the star. Initially, the dots in an"
" area of one cm<superscript>2</superscript> are in close proximity to each "
"other and the flux (energy emitted per square centimeter per second) is "
"high. After a distance d, the volume and surface area of the balloon "
"increased causing the dots to <emphasis>spread away</emphasis> from each. "
"Consequently, the number of dots (or energy) enclosed in one "
"cm<superscript>2</superscript> has decreased as illustrated in Figure 1."
msgstr ""
"Le flux mesure le <emphasis>débit</emphasis> d'énergie qui passe par "
"cm<superscript>2</superscript> (ou n'importe quelle unité de surface) de la "
"surface d'un objet chaque seconde. Le flux détecté dépend de la distance de "
"la source qui irradie l'énergie. C'est dû au fait que l'énergie doit se "
"répandre dans un volume de l'espace avant de nous atteindre. Supposons que "
"nous avons un ballon imaginaire qui entoure une étoile. Chaque point sur le "
"ballon représente une unité d'énergie émise de l'étoile. Initialement, les "
"points dans une zone de un cm<superscript>2</superscript> sont proches les "
"uns des autres et le flux (énergie émise par centimètre carré par seconde) "
"est élevé. À une distance d, le volume et la surface du ballon augmentent, "
"faisant que les points <emphasis>s'éloignent</emphasis> les uns des autres. "
"En conséquence, le nombre de points (ou énergie) compris dans un "
"cm<superscript>2</superscript> a diminué, comme illustré sur la figure 1."

#. Tag: phrase
#. +> trunk5
#: flux.docbook:40
#, no-c-format
msgid "Figure 1"
msgstr "Figure 1"

#. Tag: para
#. +> trunk5
#: flux.docbook:44
#, no-c-format
msgid ""
"The flux is inversely proportional to distance by a simple "
"r<superscript>2</superscript> relation. Therefore, if the distance is "
"doubled, we receive 1/2<superscript>2</superscript> or 1/4th of the original"
" flux. From a fundamental standpoint, the flux is the <link linkend=\"ai-"
"luminosity\">luminosity</link> per unit area:"
msgstr ""
"Le flux est inversement proportionnel à la distance par une simple relation "
"r<superscript>2</superscript>. De ce fait, si la distance double, nous "
"recevons 1/2<superscript>2</superscript>, soit 1/4 du flux original. D'un "
"point de vue fondamental, le flux est la <link linkend=\"ai-"
"luminosity\">luminosité</link> par unité de surface."

#. Tag: para
#. +> trunk5
# unreviewed-context
#: flux.docbook:55
#, no-c-format
msgid ""
"where (4 * π * R<superscript>2</superscript>) is the surface area of a "
"sphere (or a balloon!) with a radius R. Flux is measured in "
"Watts/m<superscript>2</superscript>/s or as commonly used by astronomers: "
"Ergs/cm<superscript>2</superscript>/s. For example, the luminosity of the "
"sun is L = 3.90 * 10<superscript>26</superscript> W. That is, in one second "
"the sun radiates 3.90 * 10<superscript>26</superscript> joules of energy "
"into space. Thus, the flux we receive passing through one square centimeter "
"from the sun at a distance of one AU (1.496 * "
"10<superscript>13</superscript> cm) is:"
msgstr ""
"où (4 * π * R<superscript>2</superscript>) est la surface d'une sphère "
"(ou d'un ballon) de rayon R. L'éclairement est mesuré en "
"Watt/m<superscript>2</superscript>, ou, comme les astronomes en ont "
"l'habitude, en ergs/cm<superscript>2</superscript>. Par exemple, la "
"luminosité du Soleil est L = 3,90 * 10<superscript>26</superscript> W. Cela "
"signifie que le Soleil irradie 3,90 * 10<superscript>26</superscript> joules"
" d'énergie dans l'espace en une seconde. Ainsi, le flux que nous recevons du"
" Soleil, passant par un centimètre carré à une distance d'une UA (1,4 * "
"10<superscript>13</superscript> cm) est :"