241 lines
14 KiB
Plaintext
241 lines
14 KiB
Plaintext
# KDE3 - kstars_magnitude.pot Russian translation
|
||
# translation of kstars_magnitude.po to Russian
|
||
# Copyright (C) 2004, 2005 Free Software Foundation, Inc.
|
||
#
|
||
# Valia V. Vaneeva <fattie@altlinux.ru>, 2004.
|
||
# Nick Shaforostoff <shafff@ukr.net>, 2004,2005, maintainance.
|
||
# Nick Shaforostoff <shaforostoff@kde.ru>, 2008.
|
||
# Alexander Potashev <aspotashev@gmail.com>, 2010.
|
||
msgid ""
|
||
msgstr ""
|
||
"Project-Id-Version: kstars_magnitude\n"
|
||
"Report-Msgid-Bugs-To: https://bugs.kde.org\n"
|
||
"POT-Creation-Date: 2021-03-28 16:23+0000\n"
|
||
"PO-Revision-Date: 2010-11-28 18:26+0300\n"
|
||
"Last-Translator: Alexander Potashev <aspotashev@gmail.com>\n"
|
||
"Language-Team: Russian <kde-russian@lists.kde.ru>\n"
|
||
"Language: ru\n"
|
||
"MIME-Version: 1.0\n"
|
||
"Content-Type: text/plain; charset=UTF-8\n"
|
||
"Content-Transfer-Encoding: 8bit\n"
|
||
"X-Generator: Lokalize 1.1\n"
|
||
"Plural-Forms: nplurals=4; plural=n==1 ? 3 : n%10==1 && n%100!=11 ? 0 : n"
|
||
"%10>=2 && n%10<=4 && (n%100<10 || n%100>=20) ? 1 : 2;\n"
|
||
"X-Environment: kde\n"
|
||
"X-Accelerator-Marker: \n"
|
||
"X-Text-Markup: docbook4\n"
|
||
|
||
#. Tag: author
|
||
#: magnitude.docbook:3
|
||
#, no-c-format
|
||
msgid "<firstname>Girish</firstname> <surname>V</surname>"
|
||
msgstr "<firstname>Girish</firstname> <surname>V</surname>"
|
||
|
||
#. Tag: title
|
||
#: magnitude.docbook:7
|
||
#, no-c-format
|
||
msgid "<title>Magnitude Scale</title>"
|
||
msgstr "<title>Шкала звёздных величин</title>"
|
||
|
||
#. Tag: primary
|
||
#: magnitude.docbook:8
|
||
#, no-c-format
|
||
msgid "<primary>Magnitude Scale</primary>"
|
||
msgstr "<primary>Шкала звёздных величин</primary>"
|
||
|
||
#. Tag: indexterm
|
||
#: magnitude.docbook:8
|
||
#, no-c-format
|
||
msgid "<seealso>Flux</seealso> <seealso>Star Colors and Temperatures</seealso>"
|
||
msgstr ""
|
||
"<seealso>Потоки излучения</seealso> <seealso>Цвета и температуры звёзд</"
|
||
"seealso>"
|
||
|
||
#. Tag: para
|
||
#: magnitude.docbook:12
|
||
#, no-c-format
|
||
msgid ""
|
||
"2500 years ago, the ancient Greek astronomer Hipparchus classified the "
|
||
"brightnesses of visible stars in the sky on a scale from 1 to 6. He called "
|
||
"the very brightest stars in the sky <quote>first magnitude</quote>, and the "
|
||
"very faintest stars he could see <quote>sixth magnitude</quote>. Amazingly, "
|
||
"two and a half millenia later, Hipparchus's classification scheme is still "
|
||
"widely used by astronomers, although it has since been modernized and "
|
||
"quantified."
|
||
msgstr ""
|
||
"2500 лет назад древнегреческий астроном Гиппарх классифицировал видимые "
|
||
"звёзды по яркости, используя шкалу от 1 до 6. Он назвал самые яркие звёзды "
|
||
"неба <quote>звёздами первой величины</quote>, а самые слабые из тех, которые "
|
||
"он мог видеть, — <quote>шестой величины</quote>. Удивительно, что "
|
||
"спустя две с половиной тысячи лет классификация Гиппарха все ещё широко "
|
||
"используется астрономами, хотя и была усовершенствована и переработана."
|
||
|
||
#. Tag: para
|
||
#: magnitude.docbook:20
|
||
#, no-c-format
|
||
msgid ""
|
||
"The magnitude scale runs backwards to what you might expect: brighter stars "
|
||
"have <emphasis>smaller</emphasis> magnitudes than fainter stars)."
|
||
msgstr ""
|
||
"Шкала звёздных величин идёт в направлении, обратном привычному: яркие звёзды "
|
||
"имеют <emphasis>меньшую</emphasis> величину, чем тусклые."
|
||
|
||
#. Tag: para
|
||
#: magnitude.docbook:25
|
||
#, no-c-format
|
||
msgid ""
|
||
"The modern magnitude scale is a quantitative measurement of the "
|
||
"<firstterm>flux</firstterm> of light coming from a star, with a logarithmic "
|
||
"scaling:"
|
||
msgstr ""
|
||
"Современная шкала величин представляет собой количественную меру "
|
||
"<firstterm>потока</firstterm> света от звезды по логарифмической шкале:"
|
||
|
||
#. Tag: para
|
||
#: magnitude.docbook:29
|
||
#, no-c-format
|
||
msgid "m = m<subscript>0</subscript> - 2.5 log (F / F<subscript>0</subscript>)"
|
||
msgstr ""
|
||
|
||
#. Tag: para
|
||
#: magnitude.docbook:31
|
||
#, fuzzy, no-c-format
|
||
#| msgid ""
|
||
#| "If you do not understand the math, this just says that the magnitude of a "
|
||
#| "given star (m) is different from that of some standard star (m_0) by 2.5 "
|
||
#| "times the logarithm of their flux ratio. The 2.5 *log factor means that "
|
||
#| "if the flux ratio is 100, the difference in magnitudes is 5 mag. So, a "
|
||
#| "6th magnitude star is 100 times fainter than a 1st magnitude star. The "
|
||
#| "reason Hipparchus's simple classification translates to a relatively "
|
||
#| "complex function is that the human eye responds logarithmically to light."
|
||
msgid ""
|
||
"If you do not understand the math, this just says that the magnitude of a "
|
||
"given star (m) is different from that of some standard star (m<subscript>0</"
|
||
"subscript>) by 2.5 times the logarithm of their flux ratio. The 2.5 *log "
|
||
"factor means that if the flux ratio is 100, the difference in magnitudes is "
|
||
"5 mag. So, a 6th magnitude star is 100 times fainter than a 1st magnitude "
|
||
"star. The reason Hipparchus's simple classification translates to a "
|
||
"relatively complex function is that the human eye responds logarithmically "
|
||
"to light."
|
||
msgstr ""
|
||
"Проще говоря, величина звезды (m) отличается от некой стандартной величины "
|
||
"(m_0) на логарифм отношения их потоков, умноженный на 2,5 . Этот коэффициент "
|
||
"и логарифм приводят к тому, что разница в потоке в 100 раз дает разницу в 5 "
|
||
"звёздных величин. То есть звезда шестой величины в 100 раз слабее звезды "
|
||
"первой величины. Простая классификация Гиппарха использует относительно "
|
||
"сложную функцию, потому что глаз человека именно так реагирует на яркость "
|
||
"света."
|
||
|
||
#. Tag: para
|
||
#: magnitude.docbook:40
|
||
#, no-c-format
|
||
msgid ""
|
||
"There are several different magnitude scales in use, each of which serves a "
|
||
"different purpose. The most common is the apparent magnitude scale; this is "
|
||
"just the measure of how bright stars (and other objects) look to the human "
|
||
"eye. The apparent magnitude scale defines the star Vega to have magnitude "
|
||
"0.0, and assigns magnitudes to all other objects using the above equation, "
|
||
"and a measure of the flux ratio of each object to Vega."
|
||
msgstr ""
|
||
"Есть несколько различных шкал звёздных величин, каждая из которых служит "
|
||
"своей цели. Чаще всего используется шкала видимой звёздной величины; это "
|
||
"простая оценка того, как ярка звезда (или другой объект) для человеческого "
|
||
"глаза. Она определяет яркость звезды Вега за нулевую точку отсчета и "
|
||
"присваивает другим звездам величину на основе уравнения, приведенного выше."
|
||
|
||
#. Tag: para
|
||
#: magnitude.docbook:48
|
||
#, fuzzy, no-c-format
|
||
#| msgid ""
|
||
#| "It is difficult to understand stars using just the apparent magnitudes. "
|
||
#| "Imagine two stars in the sky with the same apparent magnitude, so they "
|
||
#| "appear to be equally bright. You cannot know just by looking if the two "
|
||
#| "have the same <emphasis>intrinsic</emphasis> brightness; it is possible "
|
||
#| "that one star is intrinsically brighter, but further away. If we knew the "
|
||
#| "distances to the stars (see the <link linkend=\"ai-parallax\">parallax</"
|
||
#| "link> article), we could account for their distances and assign "
|
||
#| "<firstterm>Absolute magnitudes</firstterm> which would reflect their "
|
||
#| "true, intrinsic brightness. The absolute magnitude is defined as the "
|
||
#| "apparent magnitude the star would have if observed from a distance of 10 "
|
||
#| "parsecs (1 parsec is 3.26 light-years, or 3.1 x 10^18 cm). The absolute "
|
||
#| "magnitude (M) can be determined from the apparent magnitude (m) and the "
|
||
#| "distance in parsecs (d) using the formula:"
|
||
msgid ""
|
||
"It is difficult to understand stars using just the apparent magnitudes. "
|
||
"Imagine two stars in the sky with the same apparent magnitude, so they "
|
||
"appear to be equally bright. You cannot know just by looking if the two have "
|
||
"the same <emphasis>intrinsic</emphasis> brightness; it is possible that one "
|
||
"star is intrinsically brighter, but further away. If we knew the distances "
|
||
"to the stars (see the <link linkend=\"ai-parallax\">parallax</link> "
|
||
"article), we could account for their distances and assign "
|
||
"<firstterm>Absolute magnitudes</firstterm> which would reflect their true, "
|
||
"intrinsic brightness. The absolute magnitude is defined as the apparent "
|
||
"magnitude the star would have if observed from a distance of 10 parsecs (1 "
|
||
"parsec is 3.26 light-years, or 3.1 x 10<superscript>18</superscript> cm). "
|
||
"The absolute magnitude (M) can be determined from the apparent magnitude (m) "
|
||
"and the distance in parsecs (d) using the formula:"
|
||
msgstr ""
|
||
"Трудно сравнивать звёзды только по видимой величине. Представьте себе, что "
|
||
"две звёзды имеют одну видимую величину, так что выглядят они одинаково. "
|
||
"Однако при взгляде на них нельзя сказать, одинаковая ли у них "
|
||
"<emphasis>собственная</emphasis> яркость, ведь возможно, что одна звезда "
|
||
"ярче другой, но расположена дальше. Если бы мы знали расстояния до звёзд "
|
||
"(см. статью <link linkend=\"ai-parallax\">Параллакс</link>), мы могли бы их "
|
||
"учесть и посчитать <firstterm>абсолютную звёздную величину</firstterm>, уже "
|
||
"отражающую собственную яркость звезды. Абсолютная величина равняется "
|
||
"относительной при условии, что звезда расположена на расстоянии 10 парсеков "
|
||
"от наблюдателя (1 парсек равен 3,26 светового года или 3,1 x 10^18 см). "
|
||
"Абсолютная величина (M) может быть подсчитана из относительной (m) при "
|
||
"расстоянии d в парсеках по формуле:"
|
||
|
||
#. Tag: para
|
||
#: magnitude.docbook:63
|
||
#, no-c-format
|
||
msgid "M = m + 5 - 5 * log(d) (note that M=m when d=10)."
|
||
msgstr "M = m + 5 - 5 * log(d) (обратите внимание, что M=m, если d=10)"
|
||
|
||
#. Tag: para
|
||
#: magnitude.docbook:65
|
||
#, no-c-format
|
||
msgid ""
|
||
"The modern magnitude scale is no longer based on the human eye; it is based "
|
||
"on photographic plates and photoelectric photometers. With telescopes, we "
|
||
"can see objects much fainter than Hipparchus could see with his unaided "
|
||
"eyes, so the magnitude scale has been extended beyond 6th magnitude. In "
|
||
"fact, the Hubble Space Telescope can image stars nearly as faint as 30th "
|
||
"magnitude, which is one <emphasis>trillion</emphasis> times fainter than "
|
||
"Vega."
|
||
msgstr ""
|
||
"Современная шкала звёздных величин уже не основывается на человеческом "
|
||
"зрении, сейчас анализируются фотоснимки и фотоэлектрические фотометры. С "
|
||
"помощью телескопов мы можем наблюдать объекты намного слабее тех, которые "
|
||
"были доступны невооруженному глазу Гиппарха, поэтому шкала была расширена. "
|
||
"Сейчас космический телескоп Хаббла может наблюдать звёзды 30 величины, то "
|
||
"есть в <emphasis>триллион</emphasis> раз слабее, чем Вега."
|
||
|
||
#. Tag: para
|
||
#: magnitude.docbook:73
|
||
#, fuzzy, no-c-format
|
||
#| msgid ""
|
||
#| "A final note: the magnitude is usually measured through a color filter of "
|
||
#| "some kind, and these magnitudes are denoted by a subscript describing the "
|
||
#| "filter (&ie;, m_V is the magnitude through a <quote>visual</quote> "
|
||
#| "filter, which is greenish; m_B is the magnitude through a blue filter; "
|
||
#| "m_pg is the photographic plate magnitude, &etc;)."
|
||
msgid ""
|
||
"A final note: the magnitude is usually measured through a color filter of "
|
||
"some kind, and these magnitudes are denoted by a subscript describing the "
|
||
"filter (&ie;, m<subscript>V</subscript> is the magnitude through a "
|
||
"<quote>visual</quote> filter, which is greenish; m<subscript>B</subscript> "
|
||
"is the magnitude through a blue filter; m<subscript>pg</subscript> is the "
|
||
"photographic plate magnitude, &etc;)."
|
||
msgstr ""
|
||
"И в заключение: величина обычно измеряется через определённый цветовой "
|
||
"фильтр, и поэтому величины подписываются в соответствии с фильтром "
|
||
"(например, m_V означает фильтр <quote>видимого</quote> излучения, в "
|
||
"основном, в зеленой части спектра; m_B — синий фильтр, m_pg — "
|
||
"яркость, вычисленную с использованием фотопластинки &etc;)."
|
||
|
||
#~ msgid "m = m_0 - 2.5 log (F / F_0)"
|
||
#~ msgstr "m = m_0 - 2,5 * log (F / F_0)"
|