{"refrec":{"BRefID":303437,"RR":"<b>van Hoof, P.A.M.; Van de Steene, G.C.; Barlow, M.J.; Exter, K.M.; Sibthorpe, B.; Ueta, T.; Peris, V.; Groenewegen, M.A.T.; Blommaert, J.A.D.L.; Cohen, M.; De Meester, W.; Ferland, G.J.; Gear, W.K.; Gomez, H.L.; Hargrave, P.C.; Huygen, E.; Ivison, R.J.; Jean, C.; Leeks, S.J.; Lim, T.L.; Olofsson, G.; Polehampton, E.T.; Regibo, S.; Royer, P.; Swinyard, B.M.; Vandenbussche, B.; Van Winckel, H.; Waelkens, C.; Walker, H.J.; Wesson, R.</b> (2010). <i>Herschel</i> images of NGC 6720: H<sub>2</sub> formation on dust grains. <i>Astron. Astrophys. 518</i>: L137. <a href=\"https://dx.doi.org/10.1051/0004-6361/201014590\" target=\"_blank\">https://dx.doi.org/10.1051/0004-6361/201014590</a>","BEntID":295731,"PublicFlag":1,"CheckedFlag":0,"wosflag":1,"vabbflag":1,"RefStringPartII":". <i>Astron. Astrophys. 518</i>: L137. <a href=\"https://dx.doi.org/10.1051/0004-6361/201014590\" target=\"_blank\">https://dx.doi.org/10.1051/0004-6361/201014590</a>","DocTypID":8,"DocType":"Journal article","MarineFlag":0,"FreshFlag":0,"BrackishFlag":0,"TerrestrialFlag":0,"Authorstring":"van Hoof, P.A.M.; Van de Steene, G.C.; Barlow, M.J.; Exter, K.M.; Sibthorpe, B.; Ueta, T.; Peris, V.; Groenewegen, M.A.T.; Blommaert, J.A.D.L.; Cohen, M.; De Meester, W.; Ferland, G.J.; Gear, W.K.; Gomez, H.L.; Hargrave, P.C.; Huygen, E.; Ivison, R.J.; Jean, C.; Leeks, S.J.; Lim, T.L.; Olofsson, G.; Polehampton, E.T.; Regibo, S.; Royer, P.; Swinyard, B.M.; Vandenbussche, B.; Van Winckel, H.; Waelkens, C.; Walker, H.J.; Wesson, R.","OrigTitleTranslFlag":0,"Authorstringtrunc":"van Hoof, P.A.M. <i>et al.</i>","Englishabstract":"<i>Herschel</i> PACS and SPIRE images have been obtained of NGC&nbsp;6720 (the&nbsp;Ring nebula). This is an evolved planetary nebula with a central star that is currently on the cooling track, due to which the outer parts of the nebula are recombining. From the PACS and SPIRE images we conclude that there is a striking resemblance between the dust distribution and the H<sub>2</sub>&nbsp;emission, which appears to be observational evidence that H<sub>2</sub>&nbsp;forms on grain surfaces. We have developed a photoionization model of the nebula with the Cloudy code which we used to determine the physical conditions of the dust and investigate possible formation scenarios for the H<sub>2</sub>. We conclude that the most plausible scenario is that the H<sub>2</sub> resides in high density knots which were formed after the recombination of the gas started when the central star entered the cooling track. Hydrodynamical instabilities due to the unusually low temperature of the recombining gas are proposed as a mechanism for forming the knots. H<sub>2</sub>&nbsp;formation in the knots is expected to be substantial after the central star underwent a strong drop in luminosity about one to two thousand years ago, and may still be ongoing at this moment, depending on the density of the knots and the properties of the grains in the knots.","AbstractOtherLang":null,"BibLvlCode":"AS","StandardTitle":"<i>Herschel</i> images of NGC 6720: H<sub>2</sub> formation on dust grains","OrigTitleLangCode":"en","OrigTitleLangCodeExtended":"eng","OrigTitleLangID":15,"DateLastModified":{"date":"2026-06-10 01:32:19.133477","timezone_type":1,"timezone":"+02:00"},"UserAccessRight":null,"UserAccID":null,"AuthorKeywords":"planetary nebulae: individual: NGC 6720 / circumstellar matter / dust, extinction / infrared: ISM / ISM: molecules","OtherDescriptors":null,"Notes":null,"AnaPub":2010,"MonPub":null,"DateUpdate":"2018-11-29","DateCreate":"2018-11-29","SecASFANote":null,"ConfID":null,"PeerRev":1,"VlizCoreFlag":1,"WoScode":"WOS:000281527200138","VABBcode":null,"OpenAcc":1,"DOI":"10.1051/0004-6361/201014590"},"refs":null,"anarec":{"AnaID":303437,"PubliDate":2010,"Pagination":"L137","XtraPublOfAnaID":null,"ISBN":null,"Volume":"518","Issue":null,"BRefMon":null,"BRefMonRR":null,"BRefXtra":null,"BRefXtraRR":null,"SerBRefID":233536,"SerRR":"Astronomy & Astrophysics (Les Ulis). 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