. "\u6CE2\u6C5F\u5EA7\u03BB\u578B\u8B8A\u661F\u662FBe\u661F\u7684\u4E00\u985E\uFF0C\u5B83\u7684\u5149\u5EA6\u632F\u5E45\u5F88\u5FAE\u5C0F\uFF0C\u53EA\u6709\u767E\u5206\u4E4B\u5E7E\u7684\u661F\u7B49\u3002\u5B83\u7684\u8B8A\u5316\u975E\u5E38\u898F\u5F8B\uFF0C\u9031\u671F\u57280.5\u81F32.0\u5929\u4E4B\u9593\uFF0C\u6700\u521D\u88AB\u63CF\u8FF0\u70BA\u9031\u671F\u6027\u7684Be\u661F\u3002\u6CE2\u6C5F\u5EA7\u03BB\u662F\u6B64\u985E\u8B8A\u661F\u7684\u539F\u5F62\uFF0C\u4E5F\u662F\u7BC4\u4F8B\u3002\u8B8A\u5316\u6B78\u56E0\u65BC\u975E\u5F91\u5411\u8108\u52D5\uFF0C\u662F\u4E0D\u5747\u52FB\u7684\u65CB\u8F49\u76E4\u6216\u6046\u661F\u672C\u8EAB\u7684\u65CB\u8F49\u3002 \u9019\u7A2E\u6046\u661F\u4E0D\u662F\u5F88\u5C11\u88AB\u5206\u985E\u5C31\u662F\u5206\u985E\u4E0D\u6B63\u78BA\u3002\u8B8A\u661F\u7E3D\u8868\u4E2D\u9084\u672A\u5206\u985E\u51FA\u6CE2\u6C5F\u5EA7\u03BB\u578B\u8B8A\u661F\uFF0C\u53EA\u6709\u4ED9\u540E\u5EA7\u03B3\u578B\u8B8A\u661F\u662FGCAS\u548CBe\u661F\u662F\u975EGCAS\u3002\u6CE2\u6C5F\u5EA7\u03BB\u672C\u8EAB\u4E5F\u88AB\u932F\u8AA4\u7684\u5217\u70BA\u4ED9\u738B\u5EA7\u03B2\u578B\u8B8A\u661F\u3002\u7F8E\u570B\u8B8A\u661F\u89C0\u6E2C\u8005\u5354\u6703\uFF08AAVSO\uFF09\u5B9A\u7FA9\u4E86\u6CE2\u6C5F\u5EA7\u03BB\u578B\u8B8A\u661F\uFF1ALERI\uFF08Lambda Eridani variable\uFF09\u3002\u5305\u62EC\u6CE2\u6C5F\u5EA7\u03BB\u5728\u5167\uFF0C16\u9846\u662F\u6CE2\u6C5F\u5EA7\u03BB\u578B\u8B8A\u661F\uFF0C5\u9846\u7591\u4F3C\uFF0C13\u9846\u8207\u5176\u5B83\u985E\u578B\u8B8A\u661F\u7D50\u5408\u5728\u4E00\u8D77\u3002"@zh . . "Una variable Lambda Eridani \u00E9s una classe d\u2019estrelles Be que mostren petites variacions d\u2019amplitud d\u2019unes quantes cent\u00E8simes de magnitud. Les variacions s\u00F3n molt regulars amb per\u00EDodes d'entre 0,5 i 2,0 dies, i inicialment es van descriure com a estrelles Be peri\u00F2diques. Lambda Eridani n\u2019\u00E9s un exemple i el prototip. Aix\u00F2 s'ha atribu\u00EFt a pulsacions no radials, discos rotatius no homogenis o a la mateixa rotaci\u00F3 de l'estrella. Aquestes estrelles poques vegades es classifiquen o es classifiquen incorrectament. El Cat\u00E0leg General d'Estrelles Variables no t\u00E9 un tipus per a variables Eridani, nom\u00E9s GCAS per a variables Gamma Cassiopeiae i estrelles Be per a estrelles variables que no s\u00F3n GCAS. El mateix \u03BB Eridani apareix incorrectament com a variable Beta Cephei. L\u2019\u00EDndex internacional d\u2019estrelles variables AAVSO defineix un tipus de variabilitat LERI, amb 16 estrelles incloses com a variables \u03BB Eri, cinc d\u2019elles nom\u00E9s sospitoses, i 13 combinades amb altres tipus de variaci\u00F3."@ca . "\u00C9toile variable de type Lambda Eridani"@fr . "Lambda Eridani-variabel"@sv . "A Lambda Eridani Variable is a class of Be stars that show small amplitude variations of a few hundredths of a magnitude. The variations are highly regular with periods between 0.5 and 2.0 days, and they were initially described as periodic Be stars. Lambda Eridani is an example and the prototype. This has been ascribed to non-radial pulsations, inhomogeneous rotating discs, or the rotation of the star itself."@en . . . . "Variable Lambda Eridani"@ca . . . "Lambda Eridani-variabeln, (LERI), \u00E4r en grupp av Be-stj\u00E4rnor som \u00E4r eruptiva variabler med sm\u00E5 f\u00F6r\u00E4ndringar i ljusstyrkan p\u00E5 n\u00E5gra hundradels magnituder och h\u00F6gst regelbundna perioder p\u00E5 mellan 0,5 och 2,0 dygn. Ursprungligen beskrevs de som kortperiodiska Be-stj\u00E4rnor. Ljusvariationerna tros bero p\u00E5 icke-radiella pulseringar i ett oregelbundet gash\u00F6lje med omkretsande material som st\u00F6tts ut fr\u00E5n stj\u00E4rnan genom dess snabba rotation."@sv . "\u041F\u0435\u0440\u0435\u043C\u0435\u0301\u043D\u043D\u044B\u0435 \u0442\u0438\u0301\u043F\u0430 \u041B\u044F\u0301\u043C\u0431\u0434\u044B \u042D\u0440\u0438\u0434\u0430\u0301\u043D\u0430 \u2014 Be-\u0437\u0432\u0435\u0437\u0434\u044B, \u043A\u043E\u0442\u043E\u0440\u044B\u0435 \u043F\u043E\u043A\u0430\u0437\u044B\u0432\u0430\u044E\u0442 \u043E\u0447\u0435\u043D\u044C \u043C\u0430\u043B\u0435\u043D\u044C\u043A\u0438\u0435, \u043D\u043E \u0438\u0441\u043A\u043B\u044E\u0447\u0438\u0442\u0435\u043B\u044C\u043D\u043E \u0440\u0435\u0433\u0443\u043B\u044F\u0440\u043D\u044B\u0435 \u0432\u0430\u0440\u0438\u0430\u0446\u0438\u0438 \u044F\u0440\u043A\u043E\u0441\u0442\u0438 \u0441 \u043F\u0435\u0440\u0438\u043E\u0434\u043E\u043C \u043E\u0442 0,4 \u0434\u043E 2 \u0434\u043D\u0435\u0439, \u0447\u0442\u043E \u043C\u043E\u0436\u0435\u0442 \u0431\u044B\u0442\u044C \u0432\u044B\u0437\u0432\u0430\u043D\u043E \u043A\u043E\u043C\u043F\u043B\u0435\u043A\u0441\u043E\u043C \u043F\u0440\u0438\u0447\u0438\u043D: \u043F\u0443\u043B\u044C\u0441\u0430\u0446\u0438\u044F\u043C\u0438 \u0438\u043B\u0438 \u0432\u0440\u0430\u0449\u0435\u043D\u0438\u0435\u043C \u0438 \u0437\u0432\u0451\u0437\u0434\u043D\u044B\u043C\u0438 \u043F\u044F\u0442\u043D\u0430\u043C\u0438. \u041F\u0440\u0438\u043C\u0435\u0440\u043E\u043C \u043F\u043E\u0434\u043E\u0431\u043D\u043E\u0439 \u0437\u0432\u0435\u0437\u0434\u044B \u044F\u0432\u043B\u044F\u0435\u0442\u0441\u044F \u0410\u0445\u0435\u0440\u043D\u0430\u0440. \u041F\u0440\u043E\u0442\u043E\u0442\u0438\u043F\u043E\u043C \u0434\u0430\u043D\u043D\u043E\u0433\u043E \u0442\u0438\u043F\u0430 \u0437\u0432\u0451\u0437\u0434 \u044F\u0432\u043B\u044F\u0435\u0442\u0441\u044F \u041B\u044F\u043C\u0431\u0434\u0430 \u042D\u0440\u0438\u0434\u0430\u043D\u0430."@ru . . . "\u6CE2\u6C5F\u5EA7\u03BB\u578B\u8B8A\u661F"@zh . "A Lambda Eridani Variable is a class of Be stars that show small amplitude variations of a few hundredths of a magnitude. The variations are highly regular with periods between 0.5 and 2.0 days, and they were initially described as periodic Be stars. Lambda Eridani is an example and the prototype. This has been ascribed to non-radial pulsations, inhomogeneous rotating discs, or the rotation of the star itself. These stars are rarely classified, or are classified incorrectly. The General Catalogue of Variable Stars does not have a type for \u03BB Eridani variables, only GCAS for Gamma Cassiopeiae variables and BE for non-GCAS Be star variables. \u03BB Eridani itself is incorrectly listed as a Beta Cephei variable. The AAVSO International Variable Star Index defines a LERI type of variability, with 16 stars included as \u03BB Eri variables, five of them only suspected, and 13 combined with other types of variation."@en . "\u6CE2\u6C5F\u5EA7\u03BB\u578B\u8B8A\u661F\u662FBe\u661F\u7684\u4E00\u985E\uFF0C\u5B83\u7684\u5149\u5EA6\u632F\u5E45\u5F88\u5FAE\u5C0F\uFF0C\u53EA\u6709\u767E\u5206\u4E4B\u5E7E\u7684\u661F\u7B49\u3002\u5B83\u7684\u8B8A\u5316\u975E\u5E38\u898F\u5F8B\uFF0C\u9031\u671F\u57280.5\u81F32.0\u5929\u4E4B\u9593\uFF0C\u6700\u521D\u88AB\u63CF\u8FF0\u70BA\u9031\u671F\u6027\u7684Be\u661F\u3002\u6CE2\u6C5F\u5EA7\u03BB\u662F\u6B64\u985E\u8B8A\u661F\u7684\u539F\u5F62\uFF0C\u4E5F\u662F\u7BC4\u4F8B\u3002\u8B8A\u5316\u6B78\u56E0\u65BC\u975E\u5F91\u5411\u8108\u52D5\uFF0C\u662F\u4E0D\u5747\u52FB\u7684\u65CB\u8F49\u76E4\u6216\u6046\u661F\u672C\u8EAB\u7684\u65CB\u8F49\u3002 \u9019\u7A2E\u6046\u661F\u4E0D\u662F\u5F88\u5C11\u88AB\u5206\u985E\u5C31\u662F\u5206\u985E\u4E0D\u6B63\u78BA\u3002\u8B8A\u661F\u7E3D\u8868\u4E2D\u9084\u672A\u5206\u985E\u51FA\u6CE2\u6C5F\u5EA7\u03BB\u578B\u8B8A\u661F\uFF0C\u53EA\u6709\u4ED9\u540E\u5EA7\u03B3\u578B\u8B8A\u661F\u662FGCAS\u548CBe\u661F\u662F\u975EGCAS\u3002\u6CE2\u6C5F\u5EA7\u03BB\u672C\u8EAB\u4E5F\u88AB\u932F\u8AA4\u7684\u5217\u70BA\u4ED9\u738B\u5EA7\u03B2\u578B\u8B8A\u661F\u3002\u7F8E\u570B\u8B8A\u661F\u89C0\u6E2C\u8005\u5354\u6703\uFF08AAVSO\uFF09\u5B9A\u7FA9\u4E86\u6CE2\u6C5F\u5EA7\u03BB\u578B\u8B8A\u661F\uFF1ALERI\uFF08Lambda Eridani variable\uFF09\u3002\u5305\u62EC\u6CE2\u6C5F\u5EA7\u03BB\u5728\u5167\uFF0C16\u9846\u662F\u6CE2\u6C5F\u5EA7\u03BB\u578B\u8B8A\u661F\uFF0C5\u9846\u7591\u4F3C\uFF0C13\u9846\u8207\u5176\u5B83\u985E\u578B\u8B8A\u661F\u7D50\u5408\u5728\u4E00\u8D77\u3002"@zh . . . . . "Les (\u00E9toiles) variables de type Lambda Eridani forment un type d'\u00E9toile Be qui montrent de l\u00E9g\u00E8res amplitudes de variation de quelques centi\u00E8mes de magnitude. Ces variations sont tr\u00E8s r\u00E9guli\u00E8res et sont d'une p\u00E9riode comprise entre 0,5 et 2,0 jours, et elles ont d'ailleurs \u00E9t\u00E9 initialement d\u00E9crites comme des \u00E9toiles Be p\u00E9riodiques. Lambda Eridani est un exemple et est le prototype de ce type de variable. Ces variations ont \u00E9t\u00E9 attribu\u00E9es \u00E0 des pulsations non-radiales, \u00E0 des disques en rotation inhomog\u00E8nes, ou encore \u00E0 la rotation en elle-m\u00EAme de l'\u00E9toile."@fr . "\u041F\u0435\u0440\u0435\u043C\u0435\u0301\u043D\u043D\u044B\u0435 \u0442\u0438\u0301\u043F\u0430 \u041B\u044F\u0301\u043C\u0431\u0434\u044B \u042D\u0440\u0438\u0434\u0430\u0301\u043D\u0430 \u2014 Be-\u0437\u0432\u0435\u0437\u0434\u044B, \u043A\u043E\u0442\u043E\u0440\u044B\u0435 \u043F\u043E\u043A\u0430\u0437\u044B\u0432\u0430\u044E\u0442 \u043E\u0447\u0435\u043D\u044C \u043C\u0430\u043B\u0435\u043D\u044C\u043A\u0438\u0435, \u043D\u043E \u0438\u0441\u043A\u043B\u044E\u0447\u0438\u0442\u0435\u043B\u044C\u043D\u043E \u0440\u0435\u0433\u0443\u043B\u044F\u0440\u043D\u044B\u0435 \u0432\u0430\u0440\u0438\u0430\u0446\u0438\u0438 \u044F\u0440\u043A\u043E\u0441\u0442\u0438 \u0441 \u043F\u0435\u0440\u0438\u043E\u0434\u043E\u043C \u043E\u0442 0,4 \u0434\u043E 2 \u0434\u043D\u0435\u0439, \u0447\u0442\u043E \u043C\u043E\u0436\u0435\u0442 \u0431\u044B\u0442\u044C \u0432\u044B\u0437\u0432\u0430\u043D\u043E \u043A\u043E\u043C\u043F\u043B\u0435\u043A\u0441\u043E\u043C \u043F\u0440\u0438\u0447\u0438\u043D: \u043F\u0443\u043B\u044C\u0441\u0430\u0446\u0438\u044F\u043C\u0438 \u0438\u043B\u0438 \u0432\u0440\u0430\u0449\u0435\u043D\u0438\u0435\u043C \u0438 \u0437\u0432\u0451\u0437\u0434\u043D\u044B\u043C\u0438 \u043F\u044F\u0442\u043D\u0430\u043C\u0438. \u041F\u0440\u0438\u043C\u0435\u0440\u043E\u043C \u043F\u043E\u0434\u043E\u0431\u043D\u043E\u0439 \u0437\u0432\u0435\u0437\u0434\u044B \u044F\u0432\u043B\u044F\u0435\u0442\u0441\u044F \u0410\u0445\u0435\u0440\u043D\u0430\u0440. \u041F\u0440\u043E\u0442\u043E\u0442\u0438\u043F\u043E\u043C \u0434\u0430\u043D\u043D\u043E\u0433\u043E \u0442\u0438\u043F\u0430 \u0437\u0432\u0451\u0437\u0434 \u044F\u0432\u043B\u044F\u0435\u0442\u0441\u044F \u041B\u044F\u043C\u0431\u0434\u0430 \u042D\u0440\u0438\u0434\u0430\u043D\u0430."@ru . . "Les (\u00E9toiles) variables de type Lambda Eridani forment un type d'\u00E9toile Be qui montrent de l\u00E9g\u00E8res amplitudes de variation de quelques centi\u00E8mes de magnitude. Ces variations sont tr\u00E8s r\u00E9guli\u00E8res et sont d'une p\u00E9riode comprise entre 0,5 et 2,0 jours, et elles ont d'ailleurs \u00E9t\u00E9 initialement d\u00E9crites comme des \u00E9toiles Be p\u00E9riodiques. Lambda Eridani est un exemple et est le prototype de ce type de variable. Ces variations ont \u00E9t\u00E9 attribu\u00E9es \u00E0 des pulsations non-radiales, \u00E0 des disques en rotation inhomog\u00E8nes, ou encore \u00E0 la rotation en elle-m\u00EAme de l'\u00E9toile. Ces \u00E9toiles sont rarement classifi\u00E9es en tant que tel, ou sont classifi\u00E9es incorrectement. Le General Catalogue of Variable Stars n'attribue pas de type pour les variables de type \u03BB Eridani, seuls sont utilis\u00E9s les types GCAS pour les variables de type Gamma Cassiopeiae et BE pour toutes les \u00E9toiles Be variables et qui ne sont pas des variables de type GCAS. \u03BB Eridani elle-m\u00EAme est incorrectement list\u00E9e comme une \u00E9toile variable de type Beta Cephei. L\u2019International Variable Star Index de l'AAVSO d\u00E9finit un type de variabilit\u00E9 LERI, qui inclut 16 \u00E9toiles comme des variables de type \u03BB Eri, cinq d'entre elles n'\u00E9tant que suspect\u00E9es, et 13 \u00E9tant combin\u00E9es avec d'autres types de variation."@fr . . "Lambda Eridani variable"@en . "Una variable Lambda Eridani \u00E9s una classe d\u2019estrelles Be que mostren petites variacions d\u2019amplitud d\u2019unes quantes cent\u00E8simes de magnitud. Les variacions s\u00F3n molt regulars amb per\u00EDodes d'entre 0,5 i 2,0 dies, i inicialment es van descriure com a estrelles Be peri\u00F2diques. Lambda Eridani n\u2019\u00E9s un exemple i el prototip. Aix\u00F2 s'ha atribu\u00EFt a pulsacions no radials, discos rotatius no homogenis o a la mateixa rotaci\u00F3 de l'estrella."@ca . . . "11223398"^^ . . . . . . . . . "\u041F\u0435\u0440\u0435\u043C\u0435\u043D\u043D\u044B\u0435 \u0442\u0438\u043F\u0430 \u041B\u044F\u043C\u0431\u0434\u044B \u042D\u0440\u0438\u0434\u0430\u043D\u0430"@ru . . . "Lambda Eridani-variabeln, (LERI), \u00E4r en grupp av Be-stj\u00E4rnor som \u00E4r eruptiva variabler med sm\u00E5 f\u00F6r\u00E4ndringar i ljusstyrkan p\u00E5 n\u00E5gra hundradels magnituder och h\u00F6gst regelbundna perioder p\u00E5 mellan 0,5 och 2,0 dygn. Ursprungligen beskrevs de som kortperiodiska Be-stj\u00E4rnor. Ljusvariationerna tros bero p\u00E5 icke-radiella pulseringar i ett oregelbundet gash\u00F6lje med omkretsande material som st\u00F6tts ut fr\u00E5n stj\u00E4rnan genom dess snabba rotation."@sv . . . . . "2718"^^ . "982862910"^^ .