dc.date.accessioned | 2022-10-26T17:05:16Z | |
dc.date.available | 2022-10-26T17:05:16Z | |
dc.date.created | 2022-10-17T11:14:57Z | |
dc.date.issued | 2022 | |
dc.identifier.citation | Tiwari, Sanjiv K. Hansteen, Viggo Haraldson De Pontieu, Bart Walter Panesar, Navdeep K. Berghmans, David . SolO/EUI Observations of Ubiquitous Fine-scale Bright Dots in an Emerging Flux Region: Comparison with a Bifrost MHD Simulation. The Astrophysical Journal (ApJ). 2022, 929(1) | |
dc.identifier.uri | http://hdl.handle.net/10852/97335 | |
dc.description.abstract | We report on the presence of numerous tiny bright dots in and around an emerging flux region (an X-ray/coronal bright point) observed with SolO's EUI/HRIEUV in 174 Å. These dots are roundish and have a diameter of 675 ± 300 km, a lifetime of 50 ± 35 s, and an intensity enhancement of 30% ± 10% above their immediate surroundings. About half of the dots remain isolated during their evolution and move randomly and slowly (<10 km s−1). The other half show extensions, appearing as a small loop or surge/jet, with intensity propagations below 30 km s−1. Many of the bigger and brighter HRIEUV dots are discernible in the SDO/AIA 171 Å channel, have significant emissivity in the temperature range of 1–2 MK, and are often located at polarity inversion lines observed in SDO/HMI LOS magnetograms. Although not as pervasive as in observations, a Bifrost MHD simulation of an emerging flux region does show dots in synthetic Fe ix/x images. These dots in the simulation show distinct Doppler signatures—blueshifts and redshifts coexist, or a redshift of the order of 10 km s−1 is followed by a blueshift of similar or higher magnitude. The synthetic images of O v/vi and Si iv lines, which represent transition region radiation, also show the dots that are observed in Fe ix/x images, often expanded in size, or extended as a loop, and always with stronger Doppler velocities (up to 100 km s−1) than that in Fe ix/x lines. Our observation and simulation results, together with the field geometry of dots in the simulation, suggest that most dots in emerging flux regions form in the lower solar atmosphere (at ≈ 1 Mm) by magnetic reconnection between emerging and preexisting/emerged magnetic field. Some dots might be manifestations of magnetoacoustic shocks through the line formation region of Fe ix/x emission. | |
dc.language | EN | |
dc.rights | Attribution 4.0 International | |
dc.rights.uri | https://creativecommons.org/licenses/by/4.0/ | |
dc.title | SolO/EUI Observations of Ubiquitous Fine-scale Bright Dots in an Emerging Flux Region: Comparison with a Bifrost MHD Simulation | |
dc.title.alternative | ENEngelskEnglishSolO/EUI Observations of Ubiquitous Fine-scale Bright Dots in an Emerging Flux Region: Comparison with a Bifrost MHD Simulation | |
dc.type | Journal article | |
dc.creator.author | Tiwari, Sanjiv K. | |
dc.creator.author | Hansteen, Viggo Haraldson | |
dc.creator.author | De Pontieu, Bart Walter | |
dc.creator.author | Panesar, Navdeep K. | |
dc.creator.author | Berghmans, David | |
cristin.unitcode | 185,15,3,40 | |
cristin.unitname | Rosseland senter for solfysikk | |
cristin.ispublished | true | |
cristin.fulltext | original | |
cristin.qualitycode | 2 | |
dc.identifier.cristin | 2061928 | |
dc.identifier.bibliographiccitation | info:ofi/fmt:kev:mtx:ctx&ctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.jtitle=The Astrophysical Journal (ApJ)&rft.volume=929&rft.spage=&rft.date=2022 | |
dc.identifier.jtitle | The Astrophysical Journal (ApJ) | |
dc.identifier.volume | 929 | |
dc.identifier.issue | 1 | |
dc.identifier.pagecount | 23 | |
dc.identifier.doi | https://doi.org/10.3847/1538-4357/ac5d46 | |
dc.subject.nvi | VDP::Astrofysikk, astronomi: 438 | |
dc.type.document | Tidsskriftartikkel | |
dc.type.peerreviewed | Peer reviewed | |
dc.source.issn | 0004-637X | |
dc.type.version | PublishedVersion | |
cristin.articleid | 103 | |
dc.relation.project | NFR/262622 | |