dc.date.accessioned | 2022-11-14T17:45:16Z | |
dc.date.available | 2022-11-14T17:45:16Z | |
dc.date.created | 2022-11-09T10:51:01Z | |
dc.date.issued | 2022 | |
dc.identifier.citation | Guevara Gomez, Juan Camilo Jafarzadeh, Shahin Wedemeyer, Sven Szydlarski, Mikolaj . Propagation of transverse waves in the solar chromosphere probed at different heights with ALMA sub-bands. Astronomy and Astrophysics (A & A). 2022, 665 | |
dc.identifier.uri | http://hdl.handle.net/10852/97580 | |
dc.description.abstract | The Atacama Large Millimeter/sub-millimeter Array (ALMA) has provided us with an excellent diagnostic tool for studies of the dynamics of the Solar chromosphere, albeit through a single receiver band at one time presently. Each ALMA band consists of four sub-bands that are comprised of several spectral channels. To date, however, the spectral domain has been neglected in favour of ensuring optimal imaging, so that time-series observations have been mostly limited to full-band data products, thereby limiting studies to a single chromospheric layer. Here, we report the first observations of a dynamical event (i.e., wave propagation) for which the ALMA Band 3 data (centred at 3 mm; 100 GHz) is split into a lower and an upper sideband. In principle, this approach is aimed at mapping slightly different layers in the Solar atmosphere. The side-band data were reduced together with the Solar ALMA Pipeline (SoAP), resulting in time series of brightness-temperature maps for each side-band. Through a phase analysis of a magnetically quiet region, where purely acoustic waves are expected to dominate, the average height difference between the two side-bands is estimated as 73 ± 16 km. Furthermore, we examined the propagation of transverse waves in small-scale bright structures by means of wavelet phase analysis between oscillations at the two atmospheric heights. We find 6% of the waves to be standing, while 54% and 46% of the remaining waves are propagating upwards and downwards, respectively, with absolute propagating speeds on the order of ≈96 km s −1 , resulting in a mean energy flux of 3800 W m 2 . | |
dc.language | EN | |
dc.rights | Attribution 4.0 International | |
dc.rights.uri | https://creativecommons.org/licenses/by/4.0/ | |
dc.title | Propagation of transverse waves in the solar chromosphere probed at different heights with ALMA sub-bands | |
dc.title.alternative | ENEngelskEnglishPropagation of transverse waves in the solar chromosphere probed at different heights with ALMA sub-bands | |
dc.type | Journal article | |
dc.creator.author | Guevara Gomez, Juan Camilo | |
dc.creator.author | Jafarzadeh, Shahin | |
dc.creator.author | Wedemeyer, Sven | |
dc.creator.author | Szydlarski, Mikolaj | |
cristin.unitcode | 185,15,3,40 | |
cristin.unitname | Rosseland senter for solfysikk | |
cristin.ispublished | true | |
cristin.fulltext | original | |
cristin.qualitycode | 2 | |
dc.identifier.cristin | 2071080 | |
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=Astronomy and Astrophysics (A & A)&rft.volume=665&rft.spage=&rft.date=2022 | |
dc.identifier.jtitle | Astronomy and Astrophysics (A & A) | |
dc.identifier.volume | 665 | |
dc.identifier.pagecount | 5 | |
dc.identifier.doi | https://doi.org/10.1051/0004-6361/202244387 | |
dc.subject.nvi | VDP::Astrofysikk, astronomi: 438 | |
dc.type.document | Tidsskriftartikkel | |
dc.type.peerreviewed | Peer reviewed | |
dc.source.issn | 0004-6361 | |
dc.type.version | PublishedVersion | |
cristin.articleid | L2 | |
dc.relation.project | NFR/262622 | |