@prefix dbpprop: .
@prefix dbpedia: .
dbpprop:variable dbpedia:Delta_Scuti_variable ,
dbpedia:Delta_Scuti_variable ,
dbpedia:Delta_Scuti_variable ,
dbpedia:Delta_Scuti_variable ,
dbpedia:Delta_Scuti_variable ,
dbpedia:Delta_Scuti_variable .
dbpedia:IK_Pegasi dbpprop:variable dbpedia:Delta_Scuti_variable .
dbpedia:Beta_Cassiopeiae dbpprop:variable dbpedia:Delta_Scuti_variable .
dbpedia:AI_Velae_star dbpprop:redirect dbpedia:Delta_Scuti_variable .
dbpedia:AI_velae_star dbpprop:redirect dbpedia:Delta_Scuti_variable .
dbpprop:variable dbpedia:Delta_Scuti_variable .
dbpedia:Sigma_Octantis dbpprop:variable dbpedia:Delta_Scuti_variable .
dbpprop:variable dbpedia:Delta_Scuti_variable ,
dbpedia:Delta_Scuti_variable ,
dbpedia:Delta_Scuti_variable .
dbpedia:Delta_Scuti_variables dbpprop:redirect dbpedia:Delta_Scuti_variable .
dbpedia:EW_Aquarii dbpprop:variable dbpedia:Delta_Scuti_variable .
dbpedia:HD_182475 dbpprop:variable dbpedia:Delta_Scuti_variable .
dbpedia:Vega dbpprop:variable dbpedia:Delta_Scuti_variable .
dbpprop:variable dbpedia:Delta_Scuti_variable .
dbpedia:Altair dbpprop:variable dbpedia:Delta_Scuti_variable .
dbpedia:Delta_Capricorni dbpprop:variable dbpedia:Delta_Scuti_variable .
dbpprop:variable dbpedia:Delta_Scuti_variable .
dbpedia:Dwarf_cepheid dbpprop:redirect dbpedia:Delta_Scuti_variable .
@prefix owl: .
dbpedia:Delta_Scuti_variable owl:sameAs .
@prefix foaf: .
@prefix ns4: .
dbpedia:Delta_Scuti_variable foaf:page ns4:Delta_Scuti_variable ;
dbpprop:reference ,
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@prefix rdfs: .
dbpedia:Delta_Scuti_variable rdfs:label "Delta-Scuti-Stern"@de ,
"Delta Scuti variable"@en ,
"Variable Delta Scuti"@ca ,
"\u041F\u0435\u0440\u0435\u043C\u0435\u043D\u043D\u0430\u044F \u0437\u0432\u0435\u0437\u0434\u0430 \u0442\u0438\u043F\u0430 \u0414\u0435\u043B\u044C\u0442\u044B \u0429\u0438\u0442\u0430"@ru ,
"Estrella variable Delta Scuti"@es ,
"Variabile Delta Scuti"@it ,
"\u76FE\u724C\u5EA7\u03B4\u8B8A\u661F"@zh ,
"Hv\u011Bzdy typu Delta Scuti"@cs ,
"Variable de type Delta Scuti"@fr ,
"Delta Scuti de\u011Fi\u015Feni"@tr ,
"Gwiazdy zmienne typu Delta Scuti"@pl ,
"Delta Scuti -t\u00E4hti"@fi ,
"Delta Scuti v\u00E1ltoz\u00F3csillag"@hu ;
dbpprop:abstract "A \u03B4 Scuti v\u00E1ltoz\u00F3csillagok, m\u00E1s n\u00E9ven t\u00F6rpe cefeid\u00E1k, AI Velae vagy AI Velorum csillagok pulz\u00E1l\u00F3 v\u00E1ltoz\u00F3csillagok, melyeknek pulz\u00E1ci\u00F3s ill. f\u00E9nyess\u00E9gv\u00E1ltoz\u00E1si peri\u00F3dusa igen r\u00F6vid, 1 \u00F3ra k\u00F6r\u00FCli. Tulajdons\u00E1gaikban az RR Lyrae v\u00E1ltoz\u00F3csillagokra hasonl\u00EDtanak. Peri\u00F3dusv\u00E1ltoz\u00E1sukban gyakran t\u00F6bb felharmonikus figyelhet\u0151 meg, amelyek kombin\u00E1ci\u00F3ja k\u00FCl\u00F6n\u00F6sen \u00F6sszetett f\u00E9nyg\u00F6rb\u00E9t eredm\u00E9nyez. A tipikus \u03B4 Scuti f\u00E9nyess\u00E9gv\u00E1ltoz\u00E1s\u00E1nak amplit\u00FAd\u00F3ja 0,003 \u2013 0,9 magnit\u00FAd\u00F3. Sz\u00EDnk\u00E9pt\u00EDpusuk rendszerint AO \u00E9s F5 k\u00F6z\u00F6tti. Ezen csillagok f\u0151sorozati vagy \u00F3ri\u00E1scsillagok, legismertebb k\u00E9pvisel\u0151ik a Vega (\u03B1 Lyrae), Denebola (\u03B2 Leonis) \u00E9s a \u03B2 Cassiopeiae."@hu ,
"Une variable de type Delta Scuti (\u00E9galement appel\u00E9e C\u00E9ph\u00E9ide naine, \u00C9toile Al Velae ou \u00C9toile Al Velorum) est une \u00E9toile variable qui pr\u00E9sente des variations de luminosit\u00E9 en raison de pulsations radiales et non-radiales de la surface de l'\u00E9toile. Les fluctuations de brillance typiques vont d'une magnitude de 0,003 \u00E0 0,9 en V, dans une p\u00E9riode de quelques heures, bien que les variations de l'amplitude de la p\u00E9riode puissent grandement varier. Habituellement, ces \u00E9toiles sont des g\u00E9antes dont le type spectral se situe entre A0 et F5 ou des \u00E9toiles de la s\u00E9quence principale. Le mod\u00E8le de ces sortes d'\u00E9toiles variables est Delta Scuti, qui pr\u00E9sente des fluctuations de luminosit\u00E9 allant d'une magnitude apparente de +4,60 \u00E0 +4,79 avec une p\u00E9riode de 4,65 heures. D'autres variables bien connues de type Delta Scuti incluent V\u00E9ga (\u03B1 Lyrae), Denebola (\u03B2 Leonis) et Caph (\u03B2 Cassiopeiae). Les \u00E9toiles Al Velorum ont une amplitude plus grande (autour de 1,2) et une p\u00E9riode de 1 \u00E0 5 heures."@fr ,
"Delta Scuti -t\u00E4hti on er\u00E4s k\u00E4\u00E4pi\u00F6kefeidien alalaji. Kirkkauden muutokset johtuvat sek\u00E4 s\u00E4teitt\u00E4isist\u00E4 ett\u00E4 ei-s\u00E4teitt\u00E4isist\u00E4 muutoksista t\u00E4hdess\u00E4. Kirkkaus vaihtelee korkeudella 0,003 -- 0,9 magnitudia V-alueella muutaman tunnin jaksoissa, kirkkaudenvaihtelun jakso ja korkeus voi vaihdella suuresti. N\u00E4m\u00E4 t\u00E4hdet ovat A0 -- F5 -tyypin p\u00E4\u00E4sarjan t\u00E4hti\u00E4 ja j\u00E4ttil\u00E4isi\u00E4. Delta Scutin kirkkaus vaihtelee +4,60 -- +4,79 jaksolla 4,65 p\u00E4iv\u00E4\u00E4. Muita t\u00E4h\u00E4n ryhm\u00E4\u00E4n kuuluvia t\u00E4hti\u00E4 ovat Denebola ja Beta Cassiopeiae sek\u00E4 Delta Serpentis."@fi ,
"Las estrellas variables Delta Scuti o cefeidas enanas son un tipo de de estrellas variables que muestran variaciones en su luminosidad debidas a pulsaciones radiales y no-radiales de su superficie. Las fluctuaciones t\u00EDpicas de brillo son de 0,003 a 0,9 magnitudes en la banda V en per\u00EDodos de unas pocas horas, aunque la amplitud y el per\u00EDodo de las fluctuaciones puede variar mucho. Se pueden considerar cefeidas de baja masa, pero a diferencia de \u00E9stas tienen m\u00FAltiples per\u00EDodos de pulsaci\u00F3n superpuestos, lo que da como resultado una curva de luz compleja. Son estrellas de Poblaci\u00F3n I de la secuencia principal, subgigantes o gigantes, de tipo espectral A0 a F6. El prototipo de estas variables es Delta Scuti, cuya magnitud aparente oscila entre +4,60 y +4,79 en un per\u00EDodo principal de 4,65 horas. Est\u00E1n muy relacionadas con las estrellas variables SX Phoenicis y las variables AI Velorum. Estas \u00FAltimas presentan mayores amplitudes \u2014en torno a 1,2 magnitudes\u2014 y un per\u00EDodo entre 1 y 5 horas."@es ,
"Gwiazdy typu Delta Scuti s\u0105 gwiazdami zmiennymi typu pulsacyjnego typ\u00F3w widmowych od A do wczesnych F (klasy jasno\u015Bci od III do V). Pulsuj\u0105 radialnie i nieradialnie w modzie p (prawdopodobnie tak\u017Ce w modzie g) z okresem pomi\u0119dzy 30 min. a 8 godzin. Ich jasno\u015B\u0107 zmienia si\u0119 o mniej ni\u017C 1 magn. Im amplituda zmian jest mniejsza, tym wi\u0119cej gwiazd tego typu jest znajdowanych. Z dotychczasowych bada\u0144 wynika, \u017Ce oko\u0142o 30% gwiazd typ\u00F3w widmowych od A2 do F0, znajduj\u0105cych si\u0119 na ci\u0105gu g\u0142\u00F3wnym diagramu Hertzsprunga-Russella (HR), to gwiazdy pulsuj\u0105ce. Gwiazdy typu delta Scuti na diagramie HR znajduj\u0105 si\u0119 w pobli\u017Cu cefeid, lub przesuwaj\u0105 si\u0119 na ci\u0105gu g\u0142\u00F3wnym w kierunku olbrzym\u00F3w. Ich okres zmian wyra\u017Anie jednak odr\u00F3\u017Cnia je od innych zmiennych pulsuj\u0105cych. Reprezentuj\u0105 przej\u015Bcie pomi\u0119dzy gwiazdami pulsuj\u0105cymi jak cefeidy z du\u017C\u0105 amplitud\u0105 pulsacji a gwiazdami pulsuj\u0105cymi nieradialnie, skupionymi w \"gor\u0119tszej\" cz\u0119\u015Bci diagramu HR. Gwiazdy del Sct dzielone s\u0105 na dwie zasadnicze podgrupy: Stare, wyewoluowane gwiazdy (II. populacji), w stadium niestabilno\u015Bci, maj\u0105ce typowe okresy zmian jasno\u015Bci (gwiazdy typu SX Phe) Masywne (masy wi\u0119ksze od dw\u00F3ch mas S\u0142o\u0144ca) gwiazdy ewoluuj\u0105ce w stadium niestabilno\u015Bci W obr\u0119bie tych grup rozr\u00F3\u017Cnia si\u0119 wiele podtyp\u00F3w charakteryzuj\u0105cych si\u0119 okresami zmian i amplitud\u0105 jasno\u015Bci. Zobacz te\u017C: podstawowe zagadnienia z zakresu astronomii"@pl ,
"\u76FE\u724C\u5EA7\u03B4\u8B8A\u661F (\u4E5F\u7A31\u70BA\u77EE\u9020\u7236\u8B8A\u661F\u3001\u8239\u5E06\u5EA7 AI)\u662F\u4E00\u7A2E\u5149\u5EA6\u6703\u56E0\u70BA\u8868\u9762\u5728\u5F91\u5411\u4E0A\u7684\u8139\u7E2E\u548C\u975E\u5F91\u5411\u8139\u7E2E\u5169\u7A2E\u539F\u56E0\u9020\u6210\u5149\u5EA6\u8B8A\u5316\u7684\u8B8A\u661F\u3002\u901A\u5E38\u8868\u9762\u5149\u5EA6\u7684\u8B8A\u5316\u57280.003\u81F30.9\u8996\u661F\u7B49\uFF0C\u5728\u53EF\u898B\u5149\u7684\u8B8A\u5316\u9031\u671F\u70BA\u6578\u5C0F\u6642\uFF0C\u96D6\u7136\u632F\u5E45\u548C\u9031\u671F\u7684\u5F71\u97FF\u53EF\u80FD\u975E\u5E38\u5927\u3002\u9019\u985E\u8B8A\u661F\u7684\u985E\u578B\u901A\u5E38\u662FA0\u81F3F5\u7684\u5DE8\u661F\u6216\u4E3B\u5E8F\u661F\u3002 \u9019\u4E00\u7A2E\u8B8A\u661F\u7684\u539F\u578B\u662F\u76FE\u724C\u5EA7\u03B4\uFF0C\u5B83\u5C55\u662F\u5728\u5149\u5EA6\u4E0A\u7684\u8B8A\u5316\u5F9E +4.60\u5230 +4.79\u7B49\uFF0C\u9031\u671F\u70BA4.65\u5C0F\u6642\u3002\u5176\u4ED6\u8457\u540D\u7684\u76FE\u724C\u5EA7\u03B4\u8B8A\u661F\u5305\u62EC\u4E94\u5E1D\u5EA7\u4E00(\u7345\u5B50\u5EA7\u03B2)\u548C\u738B\u826F\u4E00(\u4ED9\u540E\u5EA7\u03B2)\u3002\u7E54\u5973\u661F\u88AB\u61F7\u7591\u4E5F\u662F\u76FE\u724C\u5EA7\u03B4\u8B8A\u661F\uFF0C\u4F46\u662F\u5C1A\u672A\u80FD\u8B49\u5BE6\u3002"@zh ,
"Una variable Delta Scuti (tamb\u00E9 conegut com a nana cef\u00E8ida, estrella AI Velae, o estrella AI Velorum) \u00E9s una estrella variable que mostra variacions en la seva lluminositat degut a pulsacions radials i no radials de la superf\u00EDcie de l'estrella. Les fluctuacions t\u00EDpiques de la seva claror van des de 0,003 a 0,9 magnituds en V en un per\u00EDode de poques hores, per b\u00E9 que l'amplitud i un per\u00EDode de les fluctuacions poden variar molt. Les estrelles s\u00F3n normalment dels tipus A0 al F5 estrelles gegants de la seq\u00FC\u00E8ncia principal. El prototipus d'aquesta classe d'estrelles variables \u00E9s Delta Scuti, que exhibeix fluctuacions del seu esclat des de +4,60 a +4,79 en magnitud aparent amb un per\u00EDode de 4,65 hores. Altres variables Delta Scuti ben conegudes s\u00F3n Vega (\u03B1 Lyrae), Denebola (\u03B2 Leonis) i \u03B2 Cassiopeiae. Les estrelles AI Velorum tenen una amplitud major (voltant 1,2) i un per\u00EDode de 1-5 hores."@ca ,
"Una variabile Delta Scuti \u00E8 una stella variabile che cambia la propria luminosit\u00E0 a causa di pulsazioni della sua superficie, sia radiali che non radiali. Le variazioni di luminosit\u00E0 sono semi-regolari e vanno tipicamente da 0,003 a 0,9 magnitudine nel corso di alcune ore. L'ampiezza e il periodo delle variazioni pu\u00F2 cambiare parecchio. Le stelle di questo tipo sono in genere giganti o di sequenza principale di tipo spettrale da A0 a F5. Il prototipo di questo tipo di variabile \u00E8 \u03B4 Scuti, che mostra fluttuazioni di luminosit\u00E0 tra le magnitudini apparenti +4,60 e +4,79, con un periodo di 4,65 ore. Altre variabili Delta Scuti famose sono Vega, Denebola, e Caph."@it ,
"\u0424\u0430\u0439\u043B:High Amplitude Delta Scuti star. gif V-band CCD phased light curves of the High Amplitude Delta Scuti star \u041F\u0435\u0440\u0435\u043C\u0435\u043D\u043D\u0430\u044F \u0442\u0438\u043F\u0430 \u03B4 \u0429\u0438\u0442\u0430\u00A0\u2014 \u043F\u0435\u0440\u0435\u043C\u0435\u043D\u043D\u0430\u044F \u0437\u0432\u0435\u0437\u0434\u0430, \u0441\u0432\u0435\u0442\u0438\u043C\u043E\u0441\u0442\u044C \u043A\u043E\u0442\u043E\u0440\u043E\u0439 \u0440\u0435\u0437\u043A\u043E \u043C\u0435\u043D\u044F\u0435\u0442\u0441\u044F \u0438\u0437-\u0437\u0430 \u0440\u0430\u0434\u0438\u0430\u043B\u044C\u043D\u044B\u0445 \u0438 \u043D\u0435\u0440\u0430\u0434\u0438\u0430\u043B\u044C\u043D\u044B\u0445 \u043F\u0443\u043B\u044C\u0441\u0430\u0446\u0438\u0439 \u043F\u043E\u0432\u0435\u0440\u0445\u043D\u043E\u0441\u0442\u0438 \u0437\u0432\u0435\u0437\u0434\u044B. \u041E\u0431\u044B\u0447\u043D\u043E \u043A \u044D\u0442\u043E\u043C\u0443 \u0442\u0438\u043F\u0443 \u043E\u0442\u043D\u043E\u0441\u044F\u0442\u0441\u044F \u0433\u0438\u0433\u0430\u043D\u0442\u044B \u0438\u043B\u0438 \u0437\u0432\u0451\u0437\u0434\u044B \u0433\u043B\u0430\u0432\u043D\u043E\u0439 \u043F\u043E\u0441\u043B\u0435\u0434\u043E\u0432\u0430\u0442\u0435\u043B\u044C\u043D\u043E\u0441\u0442\u0438 \u0441\u043F\u0435\u043A\u0442\u0440\u0430\u043B\u044C\u043D\u043E\u0433\u043E \u043A\u043B\u0430\u0441\u0441\u0430 \u043E\u0442 A0 \u0434\u043E F5 \u0441 \u0430\u043C\u043F\u043B\u0438\u0442\u0443\u0434\u043E\u0439 \u0438\u0437\u043C\u0435\u043D\u0435\u043D\u0438\u044F \u0431\u043B\u0435\u0441\u043A\u0430 \u043E\u0442 0,003 \u0434\u043E 0,9 \u0437\u0432\u0451\u0437\u0434\u043D\u044B\u0445 \u0432\u0435\u043B\u0438\u0447\u0438\u043D \u0441 \u043F\u0435\u0440\u0438\u043E\u0434\u043E\u043C \u0432 \u043D\u0435\u0441\u043A\u043E\u043B\u044C\u043A\u043E \u0447\u0430\u0441\u043E\u0432. \u0424\u043E\u0440\u043C\u0430 \u043A\u0440\u0438\u0432\u043E\u0439 \u0431\u043B\u0435\u0441\u043A\u0430, \u043F\u0435\u0440\u0438\u043E\u0434 \u0438 \u0430\u043C\u043F\u043B\u0438\u0442\u0443\u0434\u0430 \u043E\u0431\u044B\u0447\u043D\u043E \u0441\u0438\u043B\u044C\u043D\u043E \u043C\u0435\u043D\u044F\u044E\u0442\u0441\u044F. \u041D\u0430\u0431\u043B\u044E\u0434\u0430\u044E\u0442\u0441\u044F \u043A\u0430\u043A \u0440\u0430\u0434\u0438\u0430\u043B\u044C\u043D\u044B\u0435, \u0442\u0430\u043A \u0438 \u043D\u0435\u0440\u0430\u0434\u0438\u0430\u043B\u044C\u043D\u044B\u0435 \u043F\u0443\u043B\u044C\u0441\u0430\u0446\u0438\u0438. \u0423 \u043D\u0435\u043A\u043E\u0442\u043E\u0440\u044B\u0445 \u0437\u0432\u0435\u0437\u0434 \u044D\u0442\u043E\u0433\u043E \u0442\u0438\u043F\u0430 \u043F\u0435\u0440\u0435\u043C\u0435\u043D\u043D\u043E\u0441\u0442\u044C \u0431\u043B\u0435\u0441\u043A\u0430 \u043D\u0430\u0441\u0442\u0443\u043F\u0430\u0435\u0442 \u0441\u043F\u043E\u0440\u0430\u0434\u0438\u0447\u0435\u0441\u043A\u0438 \u0438 \u0438\u043D\u043E\u0433\u0434\u0430 \u043F\u043E\u043B\u043D\u043E\u0441\u0442\u044C\u044E \u043F\u0440\u0435\u043A\u0440\u0430\u0449\u0430\u0435\u0442\u0441\u044F; \u043D\u0435 \u0438\u0441\u043A\u043B\u044E\u0447\u0435\u043D\u043E, \u0447\u0442\u043E \u044D\u0442\u043E \u0441\u043B\u0435\u0434\u0441\u0442\u0432\u0438\u0435 \u0441\u0438\u043B\u044C\u043D\u043E\u0439 \u0430\u043C\u043F\u043B\u0438\u0442\u0443\u0434\u043D\u043E\u0439 \u043C\u043E\u0434\u0443\u043B\u044F\u0446\u0438\u0438 \u0441 \u043D\u0438\u0436\u043D\u0438\u043C \u043F\u0440\u0435\u0434\u0435\u043B\u043E\u043C \u0430\u043C\u043F\u043B\u0438\u0442\u0443\u0434\u044B \u043D\u0435 \u0431\u043E\u043B\u0435\u0435 0.001. \u041A\u0440\u0438\u0432\u0430\u044F \u0438\u0437\u043C\u0435\u043D\u0435\u043D\u0438\u044F \u0431\u043B\u0435\u0441\u043A\u0430 \u044F\u0432\u043B\u044F\u0435\u0442\u0441\u044F \u043F\u043E\u0447\u0442\u0438 \u0437\u0435\u0440\u043A\u0430\u043B\u044C\u043D\u044B\u043C \u043E\u0442\u043E\u0431\u0440\u0430\u0436\u0435\u043D\u0438\u0435\u043C \u043A\u0440\u0438\u0432\u043E\u0439 \u043B\u0443\u0447\u0435\u0432\u044B\u0445 \u0441\u043A\u043E\u0440\u043E\u0441\u0442\u0435\u0439: \u043C\u0430\u043A\u0441\u0438\u043C\u0443\u043C \u0441\u043A\u043E\u0440\u043E\u0441\u0442\u0438 \u0440\u0430\u0441\u0448\u0438\u0440\u0435\u043D\u0438\u044F \u043F\u043E\u0432\u0435\u0440\u0445\u043D\u043E\u0441\u0442\u043D\u044B\u0445 \u0441\u043B\u043E\u0435\u0432 \u0437\u0432\u0435\u0437\u0434\u044B \u0437\u0430\u043F\u0430\u0437\u0434\u044B\u0432\u0430\u0435\u0442 \u043F\u043E \u043E\u0442\u043D\u043E\u0448\u0435\u043D\u0438\u044E \u043A \u043C\u0430\u043A\u0441\u0438\u043C\u0443\u043C\u0443 \u0431\u043B\u0435\u0441\u043A\u0430 \u043D\u0435 \u0431\u043E\u043B\u0435\u0435, \u0447\u0435\u043C \u043D\u0430 0.1. \u041F\u0440\u043E\u0442\u043E\u0442\u0438\u043F\u043E\u043C \u043A\u043B\u0430\u0441\u0441\u0430 \u0437\u0432\u0451\u0437\u0434 \u044F\u0432\u043B\u044F\u0435\u0442\u0441\u044F \u03B4 \u0429\u0438\u0442\u0430, \u043C\u0435\u043D\u044F\u044E\u0449\u0430\u044F \u0441\u0432\u043E\u0439 \u0431\u043B\u0435\u0441\u043A \u043E\u0442 +4,6 \u0434\u043E +4.79 \u0441 \u043F\u0435\u0440\u0438\u043E\u0434\u043E\u043C 4,65 \u0447\u0430\u0441\u0430. \u041A \u044D\u0442\u043E\u043C\u0443 \u043A\u043B\u0430\u0441\u0441\u0443 \u0437\u0432\u0451\u0437\u0434 \u0442\u0430\u043A\u0436\u0435 \u043E\u0442\u043D\u043E\u0441\u044F\u0442\u0441\u044F \u0414\u0435\u043D\u0435\u0431\u043E\u043B\u0430 (\u03B2 \u041B\u044C\u0432\u0430) \u0438 \u03B2 \u041A\u0430\u0441\u0441\u0438\u043E\u043F\u0435\u0438. \u041F\u0440\u0435\u0434\u043F\u043E\u043B\u0430\u0433\u0430\u0435\u0442\u0441\u044F, \u0447\u0442\u043E \u0412\u0435\u0433\u0430 (\u03B1 \u041B\u0438\u0440\u044B) \u043E\u0442\u043D\u043E\u0441\u0438\u0442\u0441\u044F \u043A \u044D\u0442\u043E\u043C\u0443 \u0442\u0438\u043F\u0443 \u043F\u0435\u0440\u0435\u043C\u0435\u043D\u043D\u044B\u0445 \u0437\u0432\u0451\u0437\u0434."@ru ,
"Hv\u011Bzdy typu Delta Scuti jsou skupina prom\u011Bnn\u00FDch hv\u011Bzd z galaktick\u00E9ho disku s amplitudou zm\u011Bn a\u017E 0,9 mag a periodou m\u00E9n\u011B ne\u017E 2 dny. Delta Scuti jsou pulsuj\u00EDc\u00ED prom\u011Bnn\u00E9 hv\u011Bzdy spektr\u00E1ln\u00EDch typ\u016F od A do prvn\u00EDch F se t\u0159\u00EDdou sv\u011Btelnosti V a\u017E III. Pulsuj\u00ED v radi\u00E1ln\u00EDm nebo neradialn\u00EDm m\u00F3du s periodou mezi 30 minutami a 8 hodinami a fotometrickou amplitudou men\u0161\u00ED ne\u017E jedna magnituda. Po b\u00EDl\u00FDch trpasl\u00EDc\u00EDch jsou druhou nejv\u00EDce po\u010Detnou skupinou pulsuj\u00EDc\u00EDch prom\u011Bnn\u00FDch hv\u011Bzd v na\u0161\u00ED Galaxii. Prototyp prom\u011Bnnosti Delta Scuti odjevil Fath. Smith tyto objekty nazval Trpasli\u010D\u00ED Cefeidy, proto\u017Ee se zd\u00E1ly b\u00FDt rozd\u00EDln\u00E9 od typu RR Lyrae p\u0159\u00EDtomnost\u00ED kov\u016F a rozd\u00EDlnou z\u00E1vislost\u00ED periody a sv\u011Btelnosti. Bessell zavedl ozna\u010Den\u00ED hv\u011Bzdy AI Velorum pro v\u0161echny objekty s amplitudou v\u011Bt\u0161\u00ED ne\u017E 0,3 mag. Breger navrhl ozna\u010Den\u00ED Delta Scuti, kter\u00E9 je pou\u017E\u00EDv\u00E1no dodnes. Na kovy chud\u00E9 podobn\u00E9 objekty se naz\u00FDvaj\u00ED hv\u011Bzdy SX Phoenicis. Trpasli\u010D\u00ED cefeidy z diskov\u00E9 populace ozna\u010Dujeme Delta Scuti vysok\u00FDch amplitud. Jejich pr\u016Fb\u011Bh pulzace se podstat\u0148\u011B li\u0161\u00ED od ob\u011Bkt\u016F s malou amplitudou. Zdaj\u00ED se, jaky by m\u011Bly pouze jeden nebo dva radialn\u00ED m\u00F3dy. Ve v\u011Bt\u0161in\u011B p\u0159\u00EDpadech osciluj\u00ED v z\u00E1kladn\u00ED nebo prvn\u00ED harmonick\u00E9 a podobaj\u00ED se sp\u00ED\u0161e klasick\u00FDm pulsuj\u00EDc\u00EDm prom\u011Bnn\u00FDm hv\u011Bzd\u00E1m jako jsou RR Lyrae nebo cefeidy. Hv\u011Bzdy typu \u03B4 Scuti maj\u00ED vz\u00E1jemnou z\u00E1vislost periody, sv\u011Btelnosti a barvy."@cs ,
"Delta-Scuti-Sterne sind pulsationsver\u00E4nderliche Sterne der Spektralklassen A2 bis F6 und der Leuchtkraftklassen V bis III. Die Perioden liegen zwischen 0,03 und 0,2 Tagen und die Amplituden zwischen 0,003 und 0,1 Gr\u00F6\u00DFenklassen. Die Pulsation verl\u00E4uft radial und nur in der Grundschwingung, in Ausnahmef\u00E4llen auch in der 1. Oberschwingung. Die Lichtkurven entsprechen einer Sinusschwingung mit ver\u00E4nderlicher Form, Periode und Amplitude. Die Delta-Scuti-Sterne liegen im Hertzsprung-Russell-Diagramm zwischen der Hauptreihe und den RR-Lyrae-Sternen. Etwa 30 % der Hauptreihensterne in den o.g. Spektralklassen sind Delta-Scuti-Sterne. Die GCVS-Systematikk\u00FCrzel f\u00FCr Delta-Scuti-Sterne sind DSCT oder DSCTC. \u00C4hnliche Eigenschaften wie die Delta-Scuti-Sterne, allerdings bei h\u00F6heren Amplituden, zeigen die Zwergcepheiden."@de ,
"A Delta Scuti variable (also known as a Dwarf Cepheid, AI Velae Star or AI Velorum Star) is a variable star which exhibits variations in its luminosity due to both radial and non-radial pulsations of the star's surface. Typical brightness fluctuations are from 0.003 to 0.9 magnitudes in V over a period of a few hours, although the amplitude and period of the fluctuations can vary greatly. The stars are usually A0 to F5 type giant or main sequence stars. The prototype of these sorts of variable stars is Delta Scuti, which exhibits brightness fluctuations from +4.60 to +4.79 in apparent magnitude with a period of 4.65 hours. Other well known Delta Scuti variables include Altair, Denebola (\u03B2 Leonis) and \u03B2 Cassiopeiae. Vega (\u03B1 Lyrae) is a suspected Delta Scuti variable, but this remains unconfirmed."@en ,
"Delta Scuti de\u011Fi\u015Fenleri (\u03B4 Scuti), d\u00F6nemleri 0.3 g\u00FCnden k\u0131sa, A veya F tayf t\u00FCr\u00FCnden, birka\u00E7 0.001 kadirden 0.8 kadire kadar g\u00F6rsel b\u00F6lge genliklerine sahip zonklayan de\u011Fi\u015Fenlerdir. H-R diyagram\u0131ndaki karars\u0131zl\u0131k ku\u015Fa\u011F\u0131 i\u00E7inde yer al\u0131rlar. \u03B4 Scuti'lerin H-R diyagram\u0131ndaki konumlar\u0131 \u00FCstten klasik sefeler, alttan ise zonklayan beyaz c\u00FCcelerle s\u0131n\u0131rl\u0131 geni\u015F bir aland\u0131r. Bu derece geni\u015F bir alanda y\u0131ld\u0131z \u00E7e\u015Fitlili\u011Fi olduk\u00E7a fazlad\u0131r ve en gen\u00E7 disk pop\u00FClasyonlar\u0131ndan ya\u015Fl\u0131 halo y\u0131ld\u0131zlar\u0131na kadar farkl\u0131 y\u0131ld\u0131zlar \u03B4 Scuti t\u00FCr\u00FC de\u011Fi\u015Fenler grubuna girebilmektedir. Bu nedenle bir k\u0131sm\u0131 veya t\u00FCm grubu tarif eden \u00E7ok farkl\u0131 isimlerle de an\u0131l\u0131rlar; bunlardan baz\u0131lar\u0131 c\u00FCce sefeler, RRs de\u011Fi\u015Fenleri, AI Velae y\u0131ld\u0131z\u0131, SX Phe y\u0131ld\u0131zlar\u0131 ve \u00E7ok-k\u0131sa d\u00F6nemli sefeler dir."@tr ;
rdfs:comment "Una variable Delta Scuti (tamb\u00E9 conegut com a nana cef\u00E8ida, estrella AI Velae, o estrella AI Velorum) \u00E9s una estrella variable que mostra variacions en la seva lluminositat degut a pulsacions radials i no radials de la superf\u00EDcie de l'estrella. Les fluctuacions t\u00EDpiques de la seva claror van des de 0,003 a 0,9 magnituds en V en un per\u00EDode de poques hores, per b\u00E9 que l'amplitud i un per\u00EDode de les fluctuacions poden variar molt."@ca ,
""@zh ,
"Una variabile Delta Scuti \u00E8 una stella variabile che cambia la propria luminosit\u00E0 a causa di pulsazioni della sua superficie, sia radiali che non radiali. Le variazioni di luminosit\u00E0 sono semi-regolari e vanno tipicamente da 0,003 a 0,9 magnitudine nel corso di alcune ore. L'ampiezza e il periodo delle variazioni pu\u00F2 cambiare parecchio. Le stelle di questo tipo sono in genere giganti o di sequenza principale di tipo spettrale da A0 a F5."@it ,
"Gwiazdy typu Delta Scuti s\u0105 gwiazdami zmiennymi typu pulsacyjnego typ\u00F3w widmowych od A do wczesnych F (klasy jasno\u015Bci od III do V). Pulsuj\u0105 radialnie i nieradialnie w modzie p (prawdopodobnie tak\u017Ce w modzie g) z okresem pomi\u0119dzy 30 min. a 8 godzin. Ich jasno\u015B\u0107 zmienia si\u0119 o mniej ni\u017C 1 magn. Im amplituda zmian jest mniejsza, tym wi\u0119cej gwiazd tego typu jest znajdowanych."@pl ,
"Las estrellas variables Delta Scuti o cefeidas enanas son un tipo de de estrellas variables que muestran variaciones en su luminosidad debidas a pulsaciones radiales y no-radiales de su superficie. Las fluctuaciones t\u00EDpicas de brillo son de 0,003 a 0,9 magnitudes en la banda V en per\u00EDodos de unas pocas horas, aunque la amplitud y el per\u00EDodo de las fluctuaciones puede variar mucho."@es ,
"\u0424\u0430\u0439\u043B:High Amplitude Delta Scuti star. gif V-band CCD phased light curves of the High Amplitude Delta Scuti star \u041F\u0435\u0440\u0435\u043C\u0435\u043D\u043D\u0430\u044F \u0442\u0438\u043F\u0430 \u03B4 \u0429\u0438\u0442\u0430\u00A0\u2014 \u043F\u0435\u0440\u0435\u043C\u0435\u043D\u043D\u0430\u044F \u0437\u0432\u0435\u0437\u0434\u0430, \u0441\u0432\u0435\u0442\u0438\u043C\u043E\u0441\u0442\u044C \u043A\u043E\u0442\u043E\u0440\u043E\u0439 \u0440\u0435\u0437\u043A\u043E \u043C\u0435\u043D\u044F\u0435\u0442\u0441\u044F \u0438\u0437-\u0437\u0430 \u0440\u0430\u0434\u0438\u0430\u043B\u044C\u043D\u044B\u0445 \u0438 \u043D\u0435\u0440\u0430\u0434\u0438\u0430\u043B\u044C\u043D\u044B\u0445 \u043F\u0443\u043B\u044C\u0441\u0430\u0446\u0438\u0439 \u043F\u043E\u0432\u0435\u0440\u0445\u043D\u043E\u0441\u0442\u0438 \u0437\u0432\u0435\u0437\u0434\u044B."@ru ,
"A Delta Scuti variable (also known as a Dwarf Cepheid, AI Velae Star or AI Velorum Star) is a variable star which exhibits variations in its luminosity due to both radial and non-radial pulsations of the star's surface. Typical brightness fluctuations are from 0.003 to 0.9 magnitudes in V over a period of a few hours, although the amplitude and period of the fluctuations can vary greatly. The stars are usually A0 to F5 type giant or main sequence stars."@en ,
"Delta Scuti de\u011Fi\u015Fenleri (\u03B4 Scuti), d\u00F6nemleri 0.3 g\u00FCnden k\u0131sa, A veya F tayf t\u00FCr\u00FCnden, birka\u00E7 0.001 kadirden 0.8 kadire kadar g\u00F6rsel b\u00F6lge genliklerine sahip zonklayan de\u011Fi\u015Fenlerdir. H-R diyagram\u0131ndaki karars\u0131zl\u0131k ku\u015Fa\u011F\u0131 i\u00E7inde yer al\u0131rlar. \u03B4 Scuti'lerin H-R diyagram\u0131ndaki konumlar\u0131 \u00FCstten klasik sefeler, alttan ise zonklayan beyaz c\u00FCcelerle s\u0131n\u0131rl\u0131 geni\u015F bir aland\u0131r."@tr ,
"Hv\u011Bzdy typu Delta Scuti jsou skupina prom\u011Bnn\u00FDch hv\u011Bzd z galaktick\u00E9ho disku s amplitudou zm\u011Bn a\u017E 0,9 mag a periodou m\u00E9n\u011B ne\u017E 2 dny. Delta Scuti jsou pulsuj\u00EDc\u00ED prom\u011Bnn\u00E9 hv\u011Bzdy spektr\u00E1ln\u00EDch typ\u016F od A do prvn\u00EDch F se t\u0159\u00EDdou sv\u011Btelnosti V a\u017E III. Pulsuj\u00ED v radi\u00E1ln\u00EDm nebo neradialn\u00EDm m\u00F3du s periodou mezi 30 minutami a 8 hodinami a fotometrickou amplitudou men\u0161\u00ED ne\u017E jedna magnituda."@cs ,
"Delta-Scuti-Sterne sind pulsationsver\u00E4nderliche Sterne der Spektralklassen A2 bis F6 und der Leuchtkraftklassen V bis III. Die Perioden liegen zwischen 0,03 und 0,2 Tagen und die Amplituden zwischen 0,003 und 0,1 Gr\u00F6\u00DFenklassen. Die Pulsation verl\u00E4uft radial und nur in der Grundschwingung, in Ausnahmef\u00E4llen auch in der 1. Oberschwingung. Die Lichtkurven entsprechen einer Sinusschwingung mit ver\u00E4nderlicher Form, Periode und Amplitude."@de ,
"Une variable de type Delta Scuti (\u00E9galement appel\u00E9e C\u00E9ph\u00E9ide naine, \u00C9toile Al Velae ou \u00C9toile Al Velorum) est une \u00E9toile variable qui pr\u00E9sente des variations de luminosit\u00E9 en raison de pulsations radiales et non-radiales de la surface de l'\u00E9toile. Les fluctuations de brillance typiques vont d'une magnitude de 0,003 \u00E0 0,9 en V, dans une p\u00E9riode de quelques heures, bien que les variations de l'amplitude de la p\u00E9riode puissent grandement varier."@fr ,
"Delta Scuti -t\u00E4hti on er\u00E4s k\u00E4\u00E4pi\u00F6kefeidien alalaji. Kirkkauden muutokset johtuvat sek\u00E4 s\u00E4teitt\u00E4isist\u00E4 ett\u00E4 ei-s\u00E4teitt\u00E4isist\u00E4 muutoksista t\u00E4hdess\u00E4. Kirkkaus vaihtelee korkeudella 0,003 -- 0,9 magnitudia V-alueella muutaman tunnin jaksoissa, kirkkaudenvaihtelun jakso ja korkeus voi vaihdella suuresti. N\u00E4m\u00E4 t\u00E4hdet ovat A0 -- F5 -tyypin p\u00E4\u00E4sarjan t\u00E4hti\u00E4 ja j\u00E4ttil\u00E4isi\u00E4. Delta Scutin kirkkaus vaihtelee +4,60 -- +4,79 jaksolla 4,65 p\u00E4iv\u00E4\u00E4."@fi ,
"A \u03B4 Scuti v\u00E1ltoz\u00F3csillagok, m\u00E1s n\u00E9ven t\u00F6rpe cefeid\u00E1k, AI Velae vagy AI Velorum csillagok pulz\u00E1l\u00F3 v\u00E1ltoz\u00F3csillagok, melyeknek pulz\u00E1ci\u00F3s ill. f\u00E9nyess\u00E9gv\u00E1ltoz\u00E1si peri\u00F3dusa igen r\u00F6vid, 1 \u00F3ra k\u00F6r\u00FCli. Tulajdons\u00E1gaikban az RR Lyrae v\u00E1ltoz\u00F3csillagokra hasonl\u00EDtanak. Peri\u00F3dusv\u00E1ltoz\u00E1sukban gyakran t\u00F6bb felharmonikus figyelhet\u0151 meg, amelyek kombin\u00E1ci\u00F3ja k\u00FCl\u00F6n\u00F6sen \u00F6sszetett f\u00E9nyg\u00F6rb\u00E9t eredm\u00E9nyez."@hu .
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