Lehdistötiedote

Tarkat kuvat Betelgeuse-tähdestä paljastavat ylijättiläisten massanmenetyksen

Punaisen ylijättiläisen todelliset kasvot esiin

29. heinäkuuta 2009

Uudet, aiempaa tarkemmat kuvat Betelgeuse-tähdestä ovat auttaneet selvittämään mekanismin, jolla punaisiksi ylijättiläisiksi kutsutut tähdet menettävät suuria määriä massastaan. Orionin tähtikuvion toiseksi kirkkain tähti Betelgeuse on yli 1000 kertaa Aurinkoa suurempi tähti. Kaksi eri tutkimusryhmää kuvasi sitä Euroopan eteläisen observatorion (ESO) VLT (Very Large Telescope) -kaukoputkella.

Ilmakehän häiriöitä poistavan adaptiivisen optiikan ja erityisen kuvantamistekniikan yhdistelmällä saatiin aikaan kuvia, joiden terävyys lähestyy halkaisijaltaan 8-metrisen VLT-kaukoputken teoreettista rajaa. Niin kutsutussa ”lucky imaging” -tekniikassa yhdistetään useista lyhyistä valotuksista terävimmät kuvaksi, jonka laatu on parempi kuin yhdellä pitkällä valotuksella saatu. Erotuskyvyksi saatiin 37 millikaarisekuntia, mikä vastaa suunnilleen ISS-avaruusasemalla olevan tennispallon näkemistä Maasta.

Kuvista havaittiin, ettei Betelgeuse syökse materiaalia tasaisesti joka suuntaan. Sen sijaan massan menetys tapahtuu kaasupurkauksissa, joista suurin havaittu oli kuusi kertaa tähden halkaisijan pituinen, suunnilleen Auringosta Neptunukseen. Purkausten epäsymmetrialle löydettiin kaksi teoreettista mekanismia: massan menetys voisi tapahtua joko tähden navoilta pyörimisestä johtuen, tai tähden sisäisen kaasun laajamittaisen liikehdinnän seurauksena.

Kaasupurkausten syyn selvittämiseen tarvittiin vielä tarkempia kuvia. Tätä varten toinen ryhmä tähtitieteilijöitä käytti kolmea VLT:n 1,8-metristä apukaukoputkea interferometrinä ja sai otettua kuvia virtuaalisella 48-metrin kaukoputkella. Kuvien erotuskyky on neljä kertaa ensin mainitun ryhmän kuvia suurempi: se vastaa ISS-avaruusasemalla olevan marmorikuulan näkemistä Maasta.

Interferometriä käyttänyt ryhmä pääsi ensimmäisenä havainnoimaan kaasun liikkeitä jonkin muun tähden kuin Auringon pinnalla. Tutkimus paljasti, että kaasu liikkuu Betelgeusen kaasukehässä voimakkaasti ylös alas. Nämä kaasukuplat saattavat olla tähden itsensä kokoisia. Ryhmä esittääkin havaittujen massapurkausten syyksi juuri kaasun suurimittaista vellomista tähden punaisen pinnan alla.

Tulokset julkaistaan kahdessa artikkelissa Astronomy and Astrophysics -lehdessä.
ESO:n tiedote aiheesta: PR 27/09

Yhteystiedot

Pierre Kervella
Observatoire de Paris-Meudon
Paris, France
Puh.: +33 1 45 07 79 66
Sähköposti: Pierre.Kervella@obspm.fr

Keiichi Ohnaka
Max-Planck Institute for Radio Astronomy
Bonn, Germany
Puh.: +33 1 45 07 79 66
Sähköposti: kohnaka@mpifr-bonn.mpg.de

Olivier Hainaut
ESO
Garching, Germany
Puh.: +49 89 3200 6752
Sähköposti: ohainaut@eso.org

Pasi Nurmi (Lehdistön yhteyshenkilö Suomi)
ESO Science Outreach Network ja University of Turku
Turku, Finland
Puh.: +358 29 4504 358
Sähköposti: eson-finland@eso.org

Connect with ESO on social media

Tämä on ESO:n lehdistötiedotteen käännös eso0927.

Tiedotteesta

Tiedote nr.:eso0927fi
Legacy ID:PR 27/09
Nimi:Betelgeuse
Tyyppi:Milky Way : Star : Evolutionary Stage : Red Supergiant
Facility:Very Large Telescope
Instruments:AMBER, NACO, VINCI
Science data:2009A&A...504..115K
2009A&A...503..183O

Kuvat

A plume on Betelgeuse (artist’s impression)
A plume on Betelgeuse (artist’s impression)
Englanniksi
A close look at Betelgeuse
A close look at Betelgeuse
Englanniksi
Betelgeuse in Orion (with annotations)
Betelgeuse in Orion (with annotations)
Englanniksi
A plume on Betelgeuse (artist’s impression with annotations)
A plume on Betelgeuse (artist’s impression with annotations)
Englanniksi
Digitized Sky Survey image of Betelgeuse
Digitized Sky Survey image of Betelgeuse
Englanniksi

Videot

Zoom in on Betelgeuse
Zoom in on Betelgeuse
Englanniksi

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