{"id":70,"date":"2021-06-11T11:38:40","date_gmt":"2021-06-11T09:38:40","guid":{"rendered":"https:\/\/stel.asu.cas.cz\/cs\/?page_id=70"},"modified":"2026-01-28T14:13:41","modified_gmt":"2026-01-28T13:13:41","slug":"fyzika-horkych-hvezd","status":"publish","type":"page","link":"https:\/\/stel.asu.cas.cz\/cs\/fyzika-horkych-hvezd\/","title":{"rendered":"Fyzika hork\u00fdch hv\u011bzd"},"content":{"rendered":"\n<p id=\"horkehvezdy\"><\/p>\n\n\n\n<figure class=\"wp-block-image\"><img loading=\"lazy\" decoding=\"async\" width=\"1000\" height=\"333\" src=\"https:\/\/stel.asu.cas.cz\/cs\/wp-content\/uploads\/2021\/06\/hot_stars-1.jpg\" alt=\"\" class=\"wp-image-128\" srcset=\"https:\/\/stel.asu.cas.cz\/cs\/wp-content\/uploads\/2021\/06\/hot_stars-1.jpg 1000w, https:\/\/stel.asu.cas.cz\/cs\/wp-content\/uploads\/2021\/06\/hot_stars-1-300x100.jpg 300w, https:\/\/stel.asu.cas.cz\/cs\/wp-content\/uploads\/2021\/06\/hot_stars-1-768x256.jpg 768w\" sizes=\"auto, (max-width: 1000px) 100vw, 1000px\" \/><figcaption class=\"wp-element-caption\">Hv\u011bzdokupa R136 uvnit\u0159 mlhoviny Tarantula (30 Doradus) ve Velk\u00e9m Magellanov\u011b oblaku obsahuje celou \u0159adu z t\u011bch nejhmotn\u011bj\u0161\u00edch a nejz\u00e1\u0159\u00edv\u011bj\u0161\u00edch hv\u011bzd, jak\u00e9 zn\u00e1me. Kredit: NASA\/ESA<\/figcaption><\/figure>\n\n\n\n<p>V\u00fdzkum pracovn\u00ed skupiny, kterou vede <a href=\"\/cs\/fyzika-horkych-hvezd\/lide\/#kraus\" data-type=\"URL\">Michaela Kraus<\/a>, je dominantn\u011b zam\u011b\u0159en na studium hmotn\u00fdch hork\u00fdch hv\u011bzd. P\u0159esn\u011bji \u0159e\u010deno, dlouhodob\u00e9 specifick\u00e9 zam\u011b\u0159en\u00ed na Be-hv\u011bzdy a hv\u011bzdy s ob\u00e1lkou ve dvojhv\u011bzdn\u00fdch syst\u00e9mech bylo roz\u0161\u00ed\u0159eno na studium hork\u00fdch hmotn\u00fdch hv\u011bzd v r\u016fzn\u00fdch stadi\u00edch v\u00fdvoje a v sou\u010dasnosti se jedn\u00e1 o hlavn\u00ed v\u00fdzkumn\u00e9 t\u00e9ma cel\u00e9 skupiny.<\/p>\n\n\n\n<p>V r\u00e1mci sv\u00e9ho v\u00fdzkumu se skupina mimo jin\u00e9 zam\u011b\u0159uje na z\u00e1\u0159iv\u00e9 hork\u00e9 hv\u011bzdy spektr\u00e1ln\u00edch typ\u016f B- a O-, hmotn\u00e9 hv\u011bzdy v p\u0159echodn\u00e9 f\u00e1zi v\u00fdvoje (nap\u0159\u00edklad Wolf-Rayetovy hv\u011bzdy), z\u00e1\u0159iv\u00e9 modr\u00e9 prom\u011bnn\u00e9 hv\u011bzdy (Luminous Blue Variables, LBVs), modr\u00e9 superobry (Blue Supergiants, BSGs), B[e] superobry (B[e]SGs), \u017elut\u00e9 hyperobry (Yellow Hypergiants, YHGs) a rud\u00e9 superobry (Red Supergiants, RSGs). Studovan\u00e9 objekty mohou b\u00fdt bu\u010f osamocen\u00e9 nebo tvo\u0159\u00ed slo\u017eku dvojhv\u011bzdy \u010di v\u00edcen\u00e1sobn\u00e9ho syst\u00e9mu. <\/p>\n\n\n\n<p>Skupina se d\u00e1le zam\u011b\u0159uje na pozorovac\u00ed a teoretick\u00fd v\u00fdzkum chemick\u00fdch proces\u016f a&nbsp;dynamiky hmoty v okol\u00ed vyvinut\u00fdch hmotn\u00fdch hv\u011bzd (v pozdn\u00edch st\u00e1di\u00edch v\u00fdvoje).<\/p>\n\n\n\n<p>Skupina prov\u00e1d\u00ed tak\u00e9 teoretick\u00fd v\u00fdzkum orientovan\u00fd na modelov\u00e1n\u00ed hv\u011bzdn\u00fdch atmosf\u00e9r s p\u0159irozen\u00fdm zam\u011b\u0159en\u00edm na hmotn\u00e9 hork\u00e9 hv\u011bzdy. Vyu\u017e\u00edv\u00e1 k tomu model NLTE (nep\u0159edpokl\u00e1daj\u00edc\u00ed lok\u00e1ln\u00ed termodynamickou rovnov\u00e1hu) hv\u011bzdn\u00fdch atmosf\u00e9r a&nbsp;hv\u011bzdn\u00e9ho v\u011btru.<\/p>\n\n\n\n<p><strong>V\u00ddZKUMN\u00c1 T\u00c9MATA SKUPINY<\/strong><\/p>\n\n\n\n<ul class=\"wp-block-list\">\n<li>hv\u011bzdn\u00e9 atmosf\u00e9ry a hv\u011bzdn\u00fd v\u00edtr, jejich modelov\u00e1n\u00ed<\/li>\n\n\n\n<li>hmotn\u00e9 hv\u011bzdy v kr\u00e1tk\u00fdch p\u0159echodov\u00fdch f\u00e1z\u00edch v\u00fdvoje<\/li>\n<\/ul>\n\n\n\n<p><strong>\u010cLENOV\u00c9 SKUPINY<\/strong><\/p>\n\n\n\n<ul class=\"wp-block-list\">\n<li><strong>V\u011bde\u010dt\u00ed pracovn\u00edci:<\/strong> <a href=\"\/cs\/fyzika-horkych-hvezd\/lide\/#kraus#kraus\">Michaela Kraus<\/a> (vedouc\u00ed), <a href=\"\/cs\/fyzika-horkych-hvezd\/lide\/#kubat\">Ji\u0159\u00ed Kub\u00e1t<\/a>, <a href=\"https:\/\/stel.asu.cas.cz\/cs\/fyzika-horkych-hvezd\/lide\/#kubatova\">Brankica Kub\u00e1tov\u00e1<\/a>, <a href=\"https:\/\/stel.asu.cas.cz\/cs\/fyzika-horkych-hvezd\/lide\/#maryeva\">Olga Maryeva<\/a>, <a href=\"https:\/\/stel.asu.cas.cz\/cs\/fyzika-horkych-hvezd\/lide\/#michalis\">Michalis Kourniotis<\/a>, <a href=\"https:\/\/stel.asu.cas.cz\/cs\/fyzika-horkych-hvezd\/lide#jelinek\">Martin Jel\u00ednek<\/a>, <a href=\"https:\/\/stel.asu.cas.cz\/cs\/fyzika-horkych-hvezd\/lide\/#simon\">Vojt\u011bch \u0160imon<\/a>, <a href=\"https:\/\/stel.asu.cas.cz\/cs\/fyzika-horkych-hvezd\/lide\/#nemeth\">P\u00e9ter N\u00e9meth<\/a><\/li>\n\n\n\n<li><strong>Emeritn\u00ed pracovn\u00edci<\/strong>: <a href=\"\/cs\/fyzika-horkych-hvezd\/lide\/#koubsky\">Pavel Koubsk\u00fd<\/a>, <a href=\"https:\/\/stel.asu.cas.cz\/en\/hotstars\/physics-of-hot-stars-members#hudec\">Ren\u00e9 Hu<\/a><a href=\"https:\/\/stel.asu.cas.cz\/Ren\u00e9 Hudec#hudec\">d<\/a><a href=\"https:\/\/stel.asu.cas.cz\/en\/hotstars\/physics-of-hot-stars-members#hudec\">ec<\/a><\/li>\n\n\n\n<li><strong>Postdoktorandi<\/strong>: <a href=\"https:\/\/stel.asu.cas.cz\/cs\/fyzika-horkych-hvezd\/lide\/#julieta\">Julieta S\u00e1nchez Arias<\/a>, <a href=\"https:\/\/stel.asu.cas.cz\/cs\/fyzika-horkych-hvezd\/lide\/#matamala\">Alex Camilo Gormaz Matamala<\/a>, <a href=\"https:\/\/stel.asu.cas.cz\/cs\/fyzika-horkych-hvezd\/lide\/#sarkar\" data-type=\"link\" data-id=\"https:\/\/stel.asu.cas.cz\/cs\/fyzika-horkych-hvezd\/lide\/#matamala\">Shilpa Sarkar<\/a><\/li>\n\n\n\n<li><strong>Doktorandi<\/strong>: <a href=\"https:\/\/stel.asu.cas.cz\/cs\/fyzika-horkych-hvezd\/lide\/#suryani\">Suryani Guha<\/a>, <a href=\"https:\/\/stel.asu.cas.cz\/cs\/fyzika-horkych-hvezd\/lide\/#pivonkova\">Kate\u0159ina Pivo\u0148kov\u00e1<\/a>, <a href=\"https:\/\/stel.asu.cas.cz\/cs\/fyzika-horkych-hvezd\/lide\/#bodnarova\" data-type=\"link\" data-id=\"https:\/\/stel.asu.cas.cz\/cs\/fyzika-horkych-hvezd\/lide\/#bodnarova\">Radoslava Bodnarov\u00e1<\/a>, <a href=\"https:\/\/stel.asu.cas.cz\/cs\/fyzika-horkych-hvezd\/lide\/#pandey\">Nilesh Pandey<\/a><\/li>\n<\/ul>\n\n\n\n<h3 class=\"wp-block-heading\" id=\"hvezdne_atmosfery\"><strong>Hv\u011bzdn\u00e9 atmosf\u00e9ry, hv\u011bzdn\u00fd v\u00edtr a jejich modelov\u00e1n\u00ed<\/strong><\/h3>\n\n\n<div class=\"wp-block-image\">\n<figure class=\"alignleft size-large is-resized\"><img loading=\"lazy\" decoding=\"async\" width=\"1000\" height=\"795\" src=\"https:\/\/stel.asu.cas.cz\/cs\/wp-content\/uploads\/2021\/07\/Orions-Belt-stars-and-Flame-Nebula.jpg\" alt=\"\" class=\"wp-image-819\" style=\"width:250px\" srcset=\"https:\/\/stel.asu.cas.cz\/cs\/wp-content\/uploads\/2021\/07\/Orions-Belt-stars-and-Flame-Nebula.jpg 1000w, https:\/\/stel.asu.cas.cz\/cs\/wp-content\/uploads\/2021\/07\/Orions-Belt-stars-and-Flame-Nebula-300x239.jpg 300w, https:\/\/stel.asu.cas.cz\/cs\/wp-content\/uploads\/2021\/07\/Orions-Belt-stars-and-Flame-Nebula-768x611.jpg 768w\" sizes=\"auto, (max-width: 1000px) 100vw, 1000px\" \/><figcaption class=\"wp-element-caption\">Orion\u016fv p\u00e1s s mlhovinou Plam\u00ednek (vlevo) a mlhovinou Ko\u0148sk\u00e1 hlava (vlevo dole). Kredit: Digitized Sky Survey, ESA\/ESO\/NASA FITS<\/figcaption><\/figure><\/div>\n\n\n<p>Teoretick\u00fd v\u00fdzkum v tomto oboru je prim\u00e1rn\u011b zam\u011b\u0159en na v\u00fdvoj sofistikovan\u00fdch k\u00f3d\u016f popisuj\u00edc\u00edch hv\u011bzdn\u00e9 atmosf\u00e9ry, modely hv\u011bzdn\u00e9ho v\u011btru a studium fyzik\u00e1ln\u00edch mechanism\u016f, kter\u00e9 \u0159\u00edd\u00ed r\u016fzn\u00e9 procesy ve hv\u011bzd\u00e1ch a jejich okol\u00ed. Jedn\u00edm z hlavn\u00edch \u00fakol\u016f v\u00fdzkumu, kter\u00fd vede <a href=\"https:\/\/stel.asu.cas.cz\/cs\/fyzika-horkych-hvezd\/lide\/#kubat\">Ji\u0159\u00ed Kub\u00e1t<\/a>, je poskytnout vylep\u0161en\u00e9 odhady ztr\u00e1t hmoty u hmotn\u00fdch hv\u011bzd s&nbsp;pou\u017eit\u00edm vlastn\u00edho pokro\u010dil\u00e9ho modelu hv\u011bzdn\u00e9 atmosf\u00e9ry (ATA code) a&nbsp;hv\u011bzdn\u00e9ho v\u011btru v\u010detn\u011b prostorov\u00fdch (3-D) jev\u016f (jak\u00fdmi jsou nesf\u00e9ri\u010dnost a&nbsp;nehomogenity hv\u011bzdn\u00e9ho v\u011btru).<\/p>\n\n\n\n<p>Dal\u0161\u00ed v\u00fdzkumn\u00e9 aktivity jsou zam\u011b\u0159eny na v\u00fdvoj k\u00f3d\u016f, kter\u00e9 umo\u017e\u0148uj\u00ed spo\u010d\u00edtat odpov\u00eddaj\u00edc\u00ed spektra v r\u016fzn\u00fdch rozsaz\u00edch vlnov\u00fdch d\u00e9lek a kter\u00e1 mohou b\u00fdt p\u0159\u00edmo porovn\u00e1na s pozorov\u00e1n\u00edm. Na z\u00e1klad\u011b takov\u00e9ho srovn\u00e1n\u00ed je mo\u017en\u00e9 odvodit relevantn\u00ed hodnoty parametr\u016f hv\u011bzd a hv\u011bzdn\u00e9ho v\u011btru, a p\u0159edev\u0161\u00edm rychlost ztr\u00e1ty hmoty u&nbsp;hmotn\u00fdch hv\u011bzd v r\u016fzn\u00fdch st\u00e1di\u00edch v\u00fdvoje a s r\u016fznou metalicitou (obsahem t\u011b\u017e\u0161\u00edch prvk\u016f). Spr\u00e1vn\u00e1 hodnota popisuj\u00edc\u00ed ztr\u00e1tu hmoty je jedn\u00edm z hlavn\u00edch parametr\u016f modelov\u00e1n\u00ed hv\u011bzdn\u00e9ho v\u00fdvoje.<\/p>\n\n\n\n<p>Krom\u011b v\u00fdvoje vlastn\u00edch k\u00f3d\u016f jsou \u010dlenov\u00e9 skupiny rovn\u011b\u017e zb\u011bhl\u00ed v pou\u017eit\u00ed podobn\u00fdch k\u00f3d\u016f pro hv\u011bzdn\u00e9 atmosf\u00e9ry a hv\u011bzdn\u00fd v\u00edtr jin\u00fdch autor\u016f (e.g., TLUSTY, SYNSPEC, PoWR a CMFGEN) stejn\u011b jako k\u00f3d\u016f popisuj\u00edc\u00edch hv\u011bzdn\u00fd v\u00fdvoj (MESA) pro kvalitativn\u00ed hv\u011bzdnou spektroskopii a anal\u00fdzu r\u016fzn\u00fdch typ\u016f hv\u011bzd.<\/p>\n\n\n\n<h3 class=\"wp-block-heading\" id=\"hmotne_hvezdy\"><strong>Hmotn\u00e9 hv\u011bzdy v kr\u00e1tk\u00fdch p\u0159echodov\u00fdch f\u00e1z\u00edch v\u00fdvoje<\/strong><\/h3>\n\n\n<div class=\"wp-block-image float:left\">\n<figure class=\"alignleft size-large is-resized\"><img loading=\"lazy\" decoding=\"async\" width=\"800\" height=\"808\" src=\"https:\/\/stel.asu.cas.cz\/cs\/wp-content\/uploads\/2021\/07\/wr124.jpg\" alt=\"\" class=\"wp-image-818\" style=\"width:250px\" srcset=\"https:\/\/stel.asu.cas.cz\/cs\/wp-content\/uploads\/2021\/07\/wr124.jpg 800w, https:\/\/stel.asu.cas.cz\/cs\/wp-content\/uploads\/2021\/07\/wr124-297x300.jpg 297w, https:\/\/stel.asu.cas.cz\/cs\/wp-content\/uploads\/2021\/07\/wr124-768x776.jpg 768w\" sizes=\"auto, (max-width: 800px) 100vw, 800px\" \/><figcaption class=\"wp-element-caption\">Mlhovina M1-67 kolem Wolf-Reyetovy hv\u011bzdy WR124. Kredit: ESA\/Hubble &amp; NASA<\/figcaption><\/figure><\/div>\n\n\n<p>Jednou z dal\u0161\u00edch oblast\u00ed z\u00e1jmu skupiny je v\u00fdzkum hmotn\u00fdch hv\u011bzd v kr\u00e1tk\u00fdch p\u0159echodov\u00fdch f\u00e1z\u00edch v\u00fdvoje. Tyto f\u00e1ze se rozd\u011bluj\u00ed na r\u016fzn\u00e9 hv\u011bzdn\u00e9 t\u0159\u00eddy: WR stars, LBVs, BSGs, B[e]SGs, YHGs a RSGs. B\u011bhem v\u0161ech t\u011bchto v\u00fdvojov\u00fdch f\u00e1z\u00ed hv\u011bzdy jev\u00ed zn\u00e1mky vysoce dynamick\u00fdch atmosf\u00e9r \u010di ob\u00e1lek a odvrhuj\u00ed zna\u010dn\u00e9 mno\u017estv\u00ed hmoty \u010dasto v s\u00e9rii mohutn\u00fdch erupc\u00ed (exploz\u00ed). Vyvr\u017een\u00e1 hmota se hromad\u00ed bu\u010f v disku \u010di ob\u00e1lce kolem hv\u011bzdy, p\u0159\u00edpadn\u011b vytv\u00e1\u0159\u00ed mlhovinu (kterou podle struktury m\u016f\u017eeme popsat jako unipol\u00e1rn\u00ed, bipol\u00e1rn\u00ed nebo multipol\u00e1rn\u00ed).<\/p>\n\n\n\n<p>V\u00fdzkum hmotn\u00fdch hv\u011bzd v p\u0159echodov\u00fdch f\u00e1z\u00edch v\u00fdvoje vede <a href=\"https:\/\/stel.asu.cas.cz\/cs\/fyzika-horkych-hvezd\/lide\/#kraus\">Michaela&nbsp;Kraus<\/a> a je zam\u011b\u0159en na v\u00fdvoj metod vhodn\u00fdch k zji\u0161\u0165ov\u00e1n\u00ed ztr\u00e1t hmoty u tohoto typu hv\u011bzd a ke zkoum\u00e1n\u00ed chemick\u00e9ho jejich v\u00fdvoje, struktury a dynamiky vyvr\u017een\u00e9ho materi\u00e1lu. Znalost mno\u017estv\u00ed hmoty, jak\u00e9 hv\u011bzdy ztr\u00e1c\u00ed v ka\u017ed\u00e9 f\u00e1zi sv\u00e9ho \u017eivota, m\u00e1 z\u00e1sadn\u00ed v\u00fdznam pro spolehlivou p\u0159edpov\u011b\u010f dal\u0161\u00edho v\u00fdvoje a pr\u016fb\u011bhu z\u00e1v\u011bre\u010dn\u00fdch f\u00e1z\u00ed \u017eivota hmotn\u00fdch hv\u011bzd.<\/p>\n\n\n\n<p>\u010clenov\u00e9 skupiny se d\u00e1le zab\u00fdvaj\u00ed studiem fyzik\u00e1ln\u00edch mechanism\u016f, kter\u00e9 mohou v\u00e9st ke ztr\u00e1t\u011b hmoty a spustit erupci (explozi), stejn\u011b jako analyzuj\u00ed chemick\u00e9 slo\u017een\u00ed, 3-D strukturu a dynamiku v\u00fdron\u016f hmoty, aby odhalili historii ztr\u00e1t hmoty u hmotn\u00fdch hv\u011bzd v p\u0159echodn\u00fdch f\u00e1z\u00edch v\u00fdvoje.<\/p>\n\n\n\n<p>Skupina kombinuje v\u00fdsledky teoretick\u00fdch model\u016f s informacemi z\u00edskan\u00fdmi pozorov\u00e1n\u00edm. Data v optick\u00e9, infra\u010derven\u00e9 a r\u00e1diov\u00e9 \u010d\u00e1sti \u010d\u00e1sti elektromagnetick\u00e9ho spektra z\u00edsk\u00e1vaj\u00ed pomoc\u00ed dalekohled\u016f o pr\u016fm\u011bru 2 a\u017e 12 metr\u016f, vyu\u017e\u00edvaj\u00ed za\u0159\u00edzen\u00ed Observato\u0159e GEMINI (North, South), Observato\u0159e Paranal (dalekohley ESO\/VLT \u2013 Very Large Telescope), teleskop\u016f APEX, Nordic Optical Telescope, Gran Telescopio de Canarias, Southern African Large Telescope, 2.2\u2011m MPI Telescope, 2.15\u2011m CASLEO Telescope a samoz\u0159ejm\u011b Perk\u016fv dalekohled v Ond\u0159ejov\u011b. Tato data jsou dopln\u011bna pozorov\u00e1n\u00edm z\u00edskan\u00fdm pomoc\u00ed dru\u017eicov\u00fdch observato\u0159\u00ed \u2013 nap\u0159\u00edklad Spitzer Space Telescope, Wide-field Infrared Survey Explorer, stejn\u011b jako fotometrick\u00fdmi \u00fadaji a&nbsp;sv\u011bteln\u00fdmi k\u0159ivkami po\u0159\u00edzen\u00fdmi v r\u00e1mci \u0159ady pozemn\u00edch p\u0159ehl\u00eddkov\u00fdch program\u016f (nap\u0159. AAVSO, ASAS).<\/p>\n\n\n\n<h3 class=\"wp-block-heading\" id=\"ave\">Astrofyzika vysok\u00fdch energi\u00ed<\/h3>\n\n\n\n<p>Ve sv\u00e9m v\u00fdzkumu se zab\u00fdv\u00e1 mimo jin\u00e9 studiem galaktick\u00fdch a extragalaktick\u00fdch zdroj\u016f z\u00e1\u0159en\u00ed s vysokou energi\u00ed a to ve viditeln\u00e9m, dalek\u00e9m ultrafialov\u00e9m, rentgenov\u00e9m a&nbsp;gama z\u00e1\u0159en\u00ed. Zam\u011b\u0159uje se na multispektr\u00e1n\u00ed anal\u00fdzu gama z\u00e1blesk\u016f (GRB) a jejich optick\u00fdch prot\u011bj\u0161k\u016f (dosvit\u016f), aktivn\u00ed j\u00e1dra galaxi\u00ed (AGN), blazary a dal\u0161\u00ed typy kosmick\u00fdch zdroj\u016f vysoce energetick\u00e9ho z\u00e1\u0159en\u00ed v\u010detn\u011b r\u016fzn\u00fdch typ\u016f rentgenov\u00fdch dvojhv\u011bzd a kataklyzmick\u00fdch prom\u011bnn\u00fdch hv\u011bzd (CV).<\/p>\n\n\n\n<p>Aby z\u00edskali pot\u0159ebn\u00e1 pozorovac\u00ed data jsou \u010dlenov\u00e9 skupiny zapojeni do v\u00fdzkumu pomoc\u00ed \u0159ady satelit\u016f pro z\u00e1\u0159en\u00ed s vysokou energi\u00ed, tak\u00e9 spolupracuj\u00ed na projektu budouc\u00ed pozemn\u00ed observato\u0159e pro sledov\u00e1n\u00ed gama z\u00e1\u0159en\u00ed \u2013 Cherenkov Telescope Array (CTA), kter\u00e1 bude um\u00edst\u011bna na dvou stanovi\u0161t\u00edch \u2013 La Palma a Paranal. Projekt CTA v&nbsp;sou\u010dasnosti po\u010d\u00edt\u00e1 s trojic\u00ed robotick\u00fdch dalekohled\u016f FRAM, kter\u00e9 budou postaveny a&nbsp;provozov\u00e1ny ve spolupr\u00e1ci mezi \u00dastavem fyziky a skupinou Astrofyziky vysok\u00fdch energi\u00ed.<\/p>\n\n\n\n<p>Na p\u016fd\u011b observato\u0159e ASU v Ond\u0159ejov\u011b skupina provozuje dvojici relativn\u011b mal\u00fdch robotick\u00fdch dalekohled\u016f \u2013 <a href=\"http:\/\/hea.asu.cas.cz\/bart\/en\/\">BART robotic telescope<\/a> o pr\u016fm\u011bru zrcadla 25 cm a <strong>D50 robotic telescope<\/strong> s prim\u00e1rn\u00edm zrcadlem o pr\u016fm\u011bru 50 cm. \u00dakolem t\u011bchto teleskop\u016f je dopln\u011bn\u00ed dru\u017eicov\u00fdch \u00fadaj\u016f o emisi v z\u00e1\u0159en\u00ed s vysokou energi\u00ed tak\u00e9 o p\u016fvodn\u00ed data ve viditeln\u00e9m oboru a to jak v p\u0159\u00edpad\u011b gama z\u00e1blesk\u016f tak kataklyzmick\u00fdch prom\u011bnn\u00fdch hv\u011bzd. A tento \u00fakol spl\u0148uj\u00ed velmi dob\u0159e \u2013 pozorov\u00e1n\u00ed optick\u00fdch prot\u011bj\u0161k\u016f z\u00e1blesk\u016f gama vy\u017eaduje velmi rychl\u00fd reak\u010dn\u00ed \u010das cel\u00e9ho syst\u00e9mu a pozorov\u00e1n\u00ed kataklyzmick\u00fdch prom\u011bnn\u00fdch hv\u011bzd je dlouhodob\u00fdm programem t\u011bchto p\u0159\u00edstroj\u016f. <\/p>\n\n\n\n<p>Skupina je zapojena do kosmick\u00fdch projekt\u016f Evropsk\u00e9 kosmick\u00e9 agentury ESA (INTEGRAL, Gaia, XEUS) a NASA (v r\u00e1mci spolupr\u00e1ce na projektu Constellation X), p\u0159edev\u0161\u00edm s c\u00edlem detekovat kosmick\u00e9 z\u00e1blesky z\u00e1\u0159en\u00ed gama (v r\u00e1mci experiment\u016f BART, D50 a BOOTES). Dal\u0161\u00ed data \u2013 jako rozs\u00e1hl\u00e9 \u0159ady pozorov\u00e1n\u00ed o d\u00e9lce a\u017e sto let \u2013 z\u00edsk\u00e1vaj\u00ed z astronomick\u00fdch archiv\u016f, co\u017e poskytuje hodnotn\u00e9 informace o dlouhodob\u00e9m chov\u00e1n\u00ed objekt\u016f z\u00e1jmu v optick\u00e9m oboru.<\/p>\n\n\n\n<p>\u010clenov\u00e9 skupiny pravideln\u011b organizuj\u00ed mezin\u00e1rodn\u00ed konference a workshopy jako nap\u0159\u00edklad AXRO (<a href=\"https:\/\/axro.cz\">International workshops on Astronomical X\u2013Ray Optics<\/a>) nebo IBWS (<a href=\"https:\/\/ibws.cz\/\">INTEGRAL\/BART workshops<\/a>) a pod\u00edlej\u00ed se na organizaci velk\u00fdch mezin\u00e1rodn\u00edch konferenc\u00ed: SPIE Europe, Frascati workshop on Multispectral behaviour of cosmic high-energy sources, Frontier objects in astrophysics.<\/p>\n\n\n\n<ul class=\"wp-block-list\">\n<li>Pozorov\u00e1n\u00ed z\u00e1blesk\u016f z\u00e1\u0159en\u00ed gama dalekohledem FRAM: <a href=\"http:\/\/lascaux.asu.cas.cz\/m\/fram-grb.html\" target=\"_blank\" rel=\"noreferrer noopener\">FRAM GRB triggered observation<\/a><\/li>\n\n\n\n<li>Pozorov\u00e1n\u00ed z\u00e1blesk\u016f z\u00e1\u0159en\u00ed gama dalekohledem D50: <a href=\"http:\/\/lascaux50.asu.cas.cz\/m\/grb-list.html\" target=\"_blank\" rel=\"noreferrer noopener\">D50 GRB triggered observation<\/a><\/li>\n<\/ul>\n","protected":false},"excerpt":{"rendered":"<p>V\u00fdzkum pracovn\u00ed skupiny, kterou vede Michaela Kraus, je dominantn\u011b zam\u011b\u0159en na studium hmotn\u00fdch hork\u00fdch hv\u011bzd. P\u0159esn\u011bji \u0159e\u010deno, dlouhodob\u00e9 specifick\u00e9 zam\u011b\u0159en\u00ed na Be-hv\u011bzdy a hv\u011bzdy s<\/p>\n","protected":false},"author":1,"featured_media":0,"parent":0,"menu_order":0,"comment_status":"closed","ping_status":"closed","template":"","meta":{"footnotes":""},"class_list":["post-70","page","type-page","status-publish","hentry"],"_links":{"self":[{"href":"https:\/\/stel.asu.cas.cz\/cs\/wp-json\/wp\/v2\/pages\/70","targetHints":{"allow":["GET"]}}],"collection":[{"href":"https:\/\/stel.asu.cas.cz\/cs\/wp-json\/wp\/v2\/pages"}],"about":[{"href":"https:\/\/stel.asu.cas.cz\/cs\/wp-json\/wp\/v2\/types\/page"}],"author":[{"embeddable":true,"href":"https:\/\/stel.asu.cas.cz\/cs\/wp-json\/wp\/v2\/users\/1"}],"replies":[{"embeddable":true,"href":"https:\/\/stel.asu.cas.cz\/cs\/wp-json\/wp\/v2\/comments?post=70"}],"version-history":[{"count":70,"href":"https:\/\/stel.asu.cas.cz\/cs\/wp-json\/wp\/v2\/pages\/70\/revisions"}],"predecessor-version":[{"id":3687,"href":"https:\/\/stel.asu.cas.cz\/cs\/wp-json\/wp\/v2\/pages\/70\/revisions\/3687"}],"wp:attachment":[{"href":"https:\/\/stel.asu.cas.cz\/cs\/wp-json\/wp\/v2\/media?parent=70"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}