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dc.contributor.authorHerbert, Carys
dc.contributor.authorFroebrich, Dirk
dc.contributor.authorVanaverbeke, Siegfried
dc.contributor.authorScholz, Aleks
dc.contributor.authorEislöffel, Jochen
dc.contributor.authorUrtly, Thomas
dc.contributor.authorWalton, Ivan L
dc.contributor.authorWiersema, Klaas
dc.contributor.authorQuinn, Nick J
dc.contributor.authorPiehler, Georg
dc.contributor.authorAimar, Mario Morales
dc.contributor.authorGarcía, Rafael Castillo
dc.contributor.authorVanmunster, Tonny
dc.contributor.authorAlfaro, Francisco C Soldán
dc.contributor.authorde la Cuesta, Faustino García
dc.contributor.authorLicchelli, Domenico
dc.contributor.authorPerez, Alex Escartin
dc.contributor.authorMañanes, Esteban Fernández
dc.contributor.authorRibes, Noelia Graciá
dc.contributor.authorGonzález, José Luis Salto
dc.contributor.authorFutcher, Stephen R L
dc.contributor.authorNelson, Tim
dc.contributor.authorDvorak, Shawn
dc.contributor.authorMoździerski, Dawid
dc.contributor.authorKotysz, Krzysztof
dc.contributor.authorMikołajczyk, Przemysław
dc.contributor.authorFleming, George
dc.contributor.authorPhillips, Mark
dc.contributor.authorVale, Tony
dc.contributor.authorDubois, Franky
dc.contributor.authorEggenstein, Heinz-Bernd
dc.contributor.authorHeald, Michael A
dc.contributor.authorLewin, Pablo
dc.contributor.authorOKeeffe, Derek
dc.contributor.authorPopowicz, Adam
dc.contributor.authorBernacki, Krzysztof
dc.contributor.authorMalcher, Andrzej
dc.contributor.authorLasota, Slawomir
dc.contributor.authorFiolka, Jerzy
dc.contributor.authorDustor, Adam
dc.contributor.authorPercy, Stephen C
dc.contributor.authorDevine, Pat
dc.contributor.authorPatel, Aashini L
dc.contributor.authorDickers, Matthew D
dc.contributor.authorDover, Lord
dc.contributor.authorGrozdanova, Ivana I
dc.contributor.authorUrquhart, James S
dc.contributor.authorLynch, Chris J R
dc.date.accessioned2024-05-16T16:00:02Z
dc.date.available2024-05-16T16:00:02Z
dc.date.issued2024-04-01
dc.identifier.citationHerbert , C , Froebrich , D , Vanaverbeke , S , Scholz , A , Eislöffel , J , Urtly , T , Walton , I L , Wiersema , K , Quinn , N J , Piehler , G , Aimar , M M , García , R C , Vanmunster , T , Alfaro , F C S , de la Cuesta , F G , Licchelli , D , Perez , A E , Mañanes , E F , Ribes , N G , González , J L S , Futcher , S R L , Nelson , T , Dvorak , S , Moździerski , D , Kotysz , K , Mikołajczyk , P , Fleming , G , Phillips , M , Vale , T , Dubois , F , Eggenstein , H-B , Heald , M A , Lewin , P , OKeeffe , D , Popowicz , A , Bernacki , K , Malcher , A , Lasota , S , Fiolka , J , Dustor , A , Percy , S C , Devine , P , Patel , A L , Dickers , M D , Dover , L , Grozdanova , I I , Urquhart , J S & Lynch , C J R 2024 , ' A survey for variable young stars with small telescopes – IX. Evolution of spot properties on YSOs in IC 5070 ' , Monthly Notices of the Royal Astronomical Society , vol. 529 , no. 4 , pp. 4856-4878 . https://doi.org/10.1093/mnras/stae812
dc.identifier.issn0035-8711
dc.identifier.otherBibtex: 10.1093/mnras/stae812
dc.identifier.otherORCID: /0000-0002-9133-7957/work/159834805
dc.identifier.urihttp://hdl.handle.net/2299/27891
dc.description© 2024 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This is an open access article distributed under the terms of the Creative Commons Attribution License (CC BY), https://creativecommons.org/licenses/by/4.0/
dc.description.abstractWe present spot properties on 32 periodic young stellar objects in IC 5070. Long term, ∼5 yr, light curves in the V, R, and I-bands are obtained through the HOYS (Hunting Outbursting Young Stars) citizen science project. These are dissected into 6 months long slices, with 3 months oversampling, to measure 234 sets of amplitudes in all filters. We fit 180 of these with reliable spot solutions. Two thirds of spot solutions are cold spots, the lowest is 2150 K below the stellar temperature. One third are warm spots that are above the stellar temperature by less than ∼2000 K. Cold and warm spots have maximum surface coverage values of 40 per cent, although only 16 per cent of warm spots are above 20 per cent surface coverage as opposed to 60 per cent of the cold spots. Warm spots are most likely caused by a combination of plages and low-density accretion columns, most common on objects without inner disc excess emission in K − W2. Five small hot spot solutions have <3 per cent coverage and are 3000–5000 K above the stellar temperature. These are attributed to accretion, and four of them occur on the same object. The majority of our objects are likely to be accreting. However, we observe very few accretion hot spots as either the accretion is not stable on our time-scale or the photometry is dominated by other features. We do not identify cyclical spot behaviour on the targets. We additionally identify and discuss a number of objects that have interesting amplitudes, phase changes, or spot properties.en
dc.format.extent23
dc.format.extent6350158
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.subjectstars: formation
dc.subjectstars: pre-main-sequence
dc.subjectstars: rotation
dc.subjectstars: star spots
dc.subjectstars: variables: T Tauri
dc.subjectAstronomy and Astrophysics
dc.subjectSpace and Planetary Science
dc.titleA survey for variable young stars with small telescopes – IX. Evolution of spot properties on YSOs in IC 5070en
dc.contributor.institutionDepartment of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research (CAR)
dc.contributor.institutionSchool of Physics, Engineering & Computer Science
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=85191995129&partnerID=8YFLogxK
rioxxterms.versionofrecord10.1093/mnras/stae812
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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