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Publications (10 of 273) Show all publications
Bahar, E., Senavci, H. V., Isik, E., Hussain, G. A. J., Kochukhov, O., Montes, D. & Xiang, Y. (2024). First Chromospheric Activity and Doppler Imaging Study of PW And Using a New Doppler Imaging Code: SpotDIPy. Astrophysical Journal, 960(1), Article ID 60.
Open this publication in new window or tab >>First Chromospheric Activity and Doppler Imaging Study of PW And Using a New Doppler Imaging Code: SpotDIPy
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2024 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 960, no 1, article id 60Article in journal (Refereed) Published
Abstract [en]

Measuring the coverage of dark spots on cool stars is important to understanding how stellar magnetic activity scales with the rotation rate and convection zone depth. In this respect, it is crucial to infer surface magnetic patterns on G and K stars, to reveal solar-like stellar dynamos in action. Molecular bands serve as invaluable indicators of cool spots on the surfaces of stars, as they play a crucial role in enabling accurate assessments of the extent of spot coverage across the stellar surface. Therefore, more reliable surface images can be obtained considering the inversion of atomic lines with molecular bands. In this context, we simultaneously carry out Doppler imaging (DI) using atomic lines as well as titanium oxide band profiles of PW And (K2 V) and also investigate chromospheric activity indicators for the first time in the literature, using high-resolution spectra. The surface spot distribution obtained from the inversion process represents both atomic line and TiO-band profiles quite accurately. The chromospheric emission is also correlated with photospheric spot coverage, except during a possible flare event during the observations. We detect frequent flare activity, using TESS photometry. We also introduce a new open-source, Python-based DI code SpotDIPy that allows performing surface reconstructions of single stars using the maximum entropy method. We test the code by comparing surface reconstruction simulations with the extensively used DoTS code. We show that the surface brightness distribution maps reconstructed via both codes using the same simulated data are consistent with each other.

Place, publisher, year, edition, pages
Institute of Physics Publishing (IOPP), 2024
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-519554 (URN)10.3847/1538-4357/ad055d (DOI)001128967000001 ()
Funder
Swedish Research Council, 2019-03548
Available from: 2024-01-09 Created: 2024-01-09 Last updated: 2024-01-09Bibliographically approved
Metcalfe, T. S., Strassmeier, K. G., Ilyin, I. V., Buzasi, D., Kochukhov, O., Ayres, T. R., . . . Ricker, G. R. (2024). Weakened Magnetic Braking in the Exoplanet Host Star 51 Peg. Astrophysical Journal Letters, 960(1), Article ID L6.
Open this publication in new window or tab >>Weakened Magnetic Braking in the Exoplanet Host Star 51 Peg
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2024 (English)In: Astrophysical Journal Letters, ISSN 2041-8205, E-ISSN 2041-8213, Vol. 960, no 1, article id L6Article in journal (Refereed) Published
Abstract [en]

The consistently low activity level of the old solar analog 51 Peg not only facilitated the discovery of the first hot Jupiter, but also led to the suggestion that the star could be experiencing a magnetic grand minimum. However, the 50 yr time series showing minimal chromospheric variability could also be associated with the onset of weakened magnetic braking (WMB), where sufficiently slow rotation disrupts cycling activity and the production of large-scale magnetic fields by the stellar dynamo, thereby shrinking the Alfven radius and inhibiting the efficient loss of angular momentum to magnetized stellar winds. In this Letter, we evaluate the magnetic evolutionary state of 51 Peg by estimating its wind braking torque. We use new spectropolarimetric measurements from the Large Binocular Telescope to reconstruct the large-scale magnetic morphology, we reanalyze archival X-ray measurements to estimate the mass-loss rate, and we detect solar-like oscillations in photometry from the Transiting Exoplanet Survey Satellite, yielding precise stellar properties from asteroseismology. Our estimate of the wind braking torque for 51 Peg clearly places it in the WMB regime, driven by changes in the mass-loss rate and the magnetic field strength and morphology that substantially exceed theoretical expectations. Although our revised stellar properties have minimal consequences for the characterization of the exoplanet, they have interesting implications for the current space weather environment of the system.

Place, publisher, year, edition, pages
Institute of Physics Publishing (IOPP), 2024
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-521203 (URN)10.3847/2041-8213/ad0a95 (DOI)001137088900001 ()
Funder
Swedish Research CouncilSwedish National Space BoardThe Royal Swedish Academy of SciencesThe European Space Agency (ESA)
Available from: 2024-01-19 Created: 2024-01-19 Last updated: 2024-01-19Bibliographically approved
Hon, M., Huber, D., Rui, N. Z., Fuller, J., Veras, D., Kuszlewicz, J. S., . . . Weiss, L. M. (2023). A close-in giant planet escapes engulfment by its star. Nature, 618(7967), 917-920
Open this publication in new window or tab >>A close-in giant planet escapes engulfment by its star
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2023 (English)In: Nature, ISSN 0028-0836, E-ISSN 1476-4687, Vol. 618, no 7967, p. 917-920Article in journal (Refereed) Published
Abstract [en]

When main-sequence stars expand into red giants, they are expected to engulf close-in planets(1-5). Until now, the absence of planets with short orbital periods around post-expansion, core-helium-burning red giants(6-8) has been interpreted as evidence that short-period planets around Sun-like stars do not survive the giant expansion phase of their host stars(9). Here we present the discovery that the giant planet 8 Ursae Minoris b(10) orbits a core-helium-burning red giant. At a distance of only 0.5 au from its host star, the planet would have been engulfed by its host star, which is predicted by standard single-star evolution to have previously expanded to a radius of 0.7 au. Given the brief lifetime of helium-burning giants, the nearly circular orbit of the planet is challenging to reconcile with scenarios in which the planet survives by having a distant orbit initially. Instead, the planet may have avoided engulfment through a stellar merger that either altered the evolution of the host star or produced 8 Ursae Minoris b as a second-generation planet(11). This system shows that core-helium-burning red giants can harbour close planets and provides evidence for the role of non-canonical stellar evolution in the extended survival of late-stage exoplanetary systems.

Place, publisher, year, edition, pages
Springer Nature, 2023
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-510350 (URN)10.1038/s41586-023-06029-0 (DOI)001022984400018 ()37380688 (PubMedID)
Funder
Australian Research Council, FT200100871Swedish Research Council, 2019-03548EU, European Research Council, 772293
Available from: 2023-08-28 Created: 2023-08-28 Last updated: 2023-08-28Bibliographically approved
Pouilly, K., Kochukhov, O., Kospal, A., Hahlin, A., Carmona, A. & Abraham, P. (2023). Accretion process, magnetic fields, and apsidal motion in the pre-main sequence binary DQ Tau. Monthly notices of the Royal Astronomical Society, 518(4), 5072-5088
Open this publication in new window or tab >>Accretion process, magnetic fields, and apsidal motion in the pre-main sequence binary DQ Tau
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2023 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 518, no 4, p. 5072-5088Article in journal (Refereed) Published
Abstract [en]

Classical T Tauri stars (CTTSs) are young stellar objects that accrete materials from their accretion disc influenced by their strong magnetic field. The magnetic pressure truncates the disc at a few stellar radii and forces the material to leave the disc plane and fall onto the stellar surface by following the magnetic field lines. However, this global scheme may be disturbed by the presence of a companion interacting gravitationally with the accreting component. This work is aiming to study the accretion and the magnetic field of the tight eccentric binary DQ Tau, composed of two equal-mass (similar to 0.6 M-circle dot) CTTSs interacting at different orbital phases. We investigated the variability of the system using a high-resolution spectroscopic and spectropolarimetric monitoring performed with ESPaDOnS at the CFHT. We provide the first ever magnetic field analysis of this system, the Zeeman-Doppler imaging revealed a stronger magnetic field for the secondary than the primary (1.2 and 0.5 kG, respectively), but the small-scale fields analysed through Zeeman intensification yielded similar strengths (about 2.5 kG). The magnetic field topology and strengths are compatible with the accretion processes on CTTSs. Both components of this system are accreting, with a change of the main accretor during the orbital motion. In addition, the system displays a strong enhancement of the mass accretion rate at periastron and apastron. We also discovered, for the first time in this system, the apsidal motion of the orbital ellipse.

Place, publisher, year, edition, pages
Oxford University Press, 2023
Keywords
accretion, accretion discs, techniques: polarimetric, techniques: spectroscopic, binaries: spectroscopic, stars: individual: DQ Tau, stars: variables: T Tauri, stars: magnetic field
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-498154 (URN)10.1093/mnras/stac3322 (DOI)000922725900016 ()
Funder
Swedish Research Council, 2019-03548Swedish National Space BoardEU, European Research Council, 716155The Royal Swedish Academy of Sciences
Available from: 2023-03-15 Created: 2023-03-15 Last updated: 2023-03-15Bibliographically approved
Metcalfe, T. S., Buzasi, D., Huber, D., Pinsonneault, M. H., van Saders, J. L., Ayres, T. R., . . . Soon, W. (2023). Asteroseismology and Spectropolarimetry of the Exoplanet Host Star Lambda Serpentis. Astronomical Journal, 166(4), Article ID 167.
Open this publication in new window or tab >>Asteroseismology and Spectropolarimetry of the Exoplanet Host Star Lambda Serpentis
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2023 (English)In: Astronomical Journal, ISSN 0004-6256, E-ISSN 1538-3881, Vol. 166, no 4, article id 167Article in journal (Refereed) Published
Abstract [en]

The bright star lambda Ser hosts a hot Neptune with a minimum mass of 13.6 M & OPLUS; and a 15.5 day orbit. It also appears to be a solar analog, with a mean rotation period of 25.8 days and surface differential rotation very similar to the Sun. We aim to characterize the fundamental properties of this system and constrain the evolutionary pathway that led to its present configuration. We detect solar-like oscillations in time series photometry from the Transiting Exoplanet Survey Satellite, and we derive precise asteroseismic properties from detailed modeling. We obtain new spectropolarimetric data, and we use them to reconstruct the large-scale magnetic field morphology. We reanalyze the complete time series of chromospheric activity measurements from the Mount Wilson Observatory, and we present new X-ray and ultraviolet observations from the Chandra and Hubble space telescopes. Finally, we use the updated observational constraints to assess the rotational history of the star and estimate the wind braking torque. We conclude that the remaining uncertainty on the stellar age currently prevents an unambiguous interpretation of the properties of lambda Ser, and that the rate of angular momentum loss appears to be higher than for other stars with a similar Rossby number. Future asteroseismic observations may help to improve the precision of the stellar age.

Place, publisher, year, edition, pages
Institute of Physics (IOP), 2023
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-515046 (URN)10.3847/1538-3881/acf1f7 (DOI)001074325400001 ()
Funder
Australian Research CouncilSwedish Research CouncilSwedish National Space BoardEU, European Research CouncilEU, European Research CouncilThe Royal Swedish Academy of SciencesThe European Space Agency (ESA)
Available from: 2023-11-03 Created: 2023-11-03 Last updated: 2023-11-03Bibliographically approved
Goffo, E., Gandolfi, D., Egger, J. A., Mustill, A. J., Albrecht, S. H., Hirano, T., . . . Winn, J. N. (2023). Company for the Ultra-high Density, Ultra-short Period Sub-Earth GJ 367 b: Discovery of Two Additional Low-mass Planets at 11.5 and 34 Days. Astrophysical Journal Letters, 955(1), Article ID L3.
Open this publication in new window or tab >>Company for the Ultra-high Density, Ultra-short Period Sub-Earth GJ 367 b: Discovery of Two Additional Low-mass Planets at 11.5 and 34 Days
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2023 (English)In: Astrophysical Journal Letters, ISSN 2041-8205, E-ISSN 2041-8213, Vol. 955, no 1, article id L3Article in journal (Refereed) Published
Abstract [en]

GJ 367 is a bright (V approximate to 10.2) M1 V star that has been recently found to host a transiting ultra-short period subEarth on a 7.7 hr orbit. With the aim of improving the planetary mass and radius and unveiling the inner architecture of the system, we performed an intensive radial velocity follow-up campaign with the HARPS spectrograph-collecting 371 high-precision measurements over a baseline of nearly 3 yr-and combined our Doppler measurements with new TESS observations from sectors 35 and 36. We found that GJ 367 b has a mass of M-b = 0.633 +/- 0.050M. and a radius of R-b = 0.699 +/- 0.024 R-circle plus, corresponding to precisions of 8% and 3.4%, respectively. This implies a planetary bulk density of rho(b) = 10.2 +/- 1.3 g cm(-3), i.e., 85% higher than Earth's density. We revealed the presence of two additional non-transiting low-mass companions with orbital periods of similar to 11.5 and 34 days and minimum masses of M-c sin i(c) = 4.13 +/- 0.36 M-circle plus and M-d sin i(d) = 6.03 +/- 0.49M(circle plus), respectively, which lie close to the 3:1 mean motion commensurability. GJ 367 b joins the small class of highdensity planets, namely the class of super-Mercuries, being the densest ultra-short period small planet known to date. Thanks to our precise mass and radius estimates, we explored the potential internal composition and structure of GJ 367 b, and found that it is expected to have an iron core with a mass fraction of 0.91(-0.23)(+0.07). How this iron core is formed and how such a high density is reached is still not clear, and we discuss the possible pathways of formation of such a small ultra-dense planet.

Place, publisher, year, edition, pages
Institute of Physics (IOP), 2023
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-515050 (URN)10.3847/2041-8213/ace0c7 (DOI)001070300000001 ()
Funder
German Research Foundation (DFG), HA3279/14-1Swedish National Space Board, DNR 65/19Swedish Research Council, 2019-03548Swedish National Space Board, DNR 2020-001Swedish Research Council, 2017-04945
Available from: 2023-11-07 Created: 2023-11-07 Last updated: 2023-11-07Bibliographically approved
Metcalfe, T. S., Strassmeier, K. G., Ilyin, I. V., van Saders, J. L., Ayres, T. R., Finley, A. J., . . . Vidotto, A. A. (2023). Constraints on Magnetic Braking from the G8 Dwarf Stars 61 UMa and tau Cet. Astrophysical Journal Letters, 948(1), Article ID L6.
Open this publication in new window or tab >>Constraints on Magnetic Braking from the G8 Dwarf Stars 61 UMa and tau Cet
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2023 (English)In: Astrophysical Journal Letters, ISSN 2041-8205, E-ISSN 2041-8213, Vol. 948, no 1, article id L6Article in journal (Refereed) Published
Abstract [en]

During the first half of their main-sequence lifetimes, stars rapidly lose angular momentum to their magnetized winds, a process known as magnetic braking. Recent observations suggest a substantial decrease in the magnetic braking efficiency when stars reach a critical value of the Rossby number, the stellar rotation period normalized by the convective overturn timescale. Cooler stars have deeper convection zones with longer overturn times, reaching this critical Rossby number at slower rotation rates. The nature and timing of the transition to weakened magnetic braking have previously been constrained by several solar analogs and two slightly hotter stars. In this Letter, we derive the first direct constraints from stars cooler than the Sun. We present new spectropolarimetry of the old G8 dwarf tau Cet from the Large Binocular Telescope, and we reanalyze a published Zeeman Doppler image of the younger G8 star 61 UMa, yielding the large-scale magnetic field strengths and morphologies. We estimate mass-loss rates using archival X-ray observations and inferences from Ly alpha measurements, and we adopt other stellar properties from asteroseismology and spectral energy distribution fitting. The resulting calculations of the wind braking torque demonstrate that the rate of angular momentum loss drops by a factor of 300 between the ages of these two stars (1.4-9 Gyr), well above theoretical expectations. We summarize the available data to help constrain the value of the critical Rossby number, and we identify a new signature of the long-period detection edge in recent measurements from the Kepler mission.

Place, publisher, year, edition, pages
Institute of Physics (IOP), 2023
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-503656 (URN)10.3847/2041-8213/acce38 (DOI)000978163600001 ()
Funder
EU, Horizon 2020, 810218 WHOLESUNSwedish Research Council, 2019-03548EU, Horizon 2020, 817540 ASTROFLOWThe Royal Swedish Academy of Sciences
Available from: 2023-06-09 Created: 2023-06-09 Last updated: 2023-06-09Bibliographically approved
Yan, F., Nortmann, L., Reiners, A., Piskunov, N., Hatzes, A., Seemann, U., . . . Stempels, H. C. (2023). CRIRES+ detection of CO emissions lines and temperature inversions on the dayside of WASP-18b and WASP-76b. Astronomy and Astrophysics, 672, Article ID A107.
Open this publication in new window or tab >>CRIRES+ detection of CO emissions lines and temperature inversions on the dayside of WASP-18b and WASP-76b
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2023 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 672, article id A107Article in journal (Refereed) Published
Abstract [en]

The dayside atmospheres of ultra-hot Jupiters (UHJs) are predicted to possess temperature inversion layers with extremely high temperatures at high altitudes. We observed the dayside thermal emission spectra of WASP-18b and WASP-76b with the new CRIRES+ high-resolution spectrograph at near-infrared wavelengths. Using the cross-correlation technique, we detected strong CO emission lines in both planets, which confirms the existence of temperature inversions on their dayside hemispheres. The two planets are the first UHJs orbiting F-type stars with CO emission lines detected; previous detections were mostly for UHJs orbiting A-type stars. Evidence of weak H2O emission signals is also found for both planets. We further applied forward-model retrievals on the detected CO lines and retrieved the temperature-pressure profiles along with the CO volume mixing ratios. The retrieved logarithmic CO mixing ratio of WASP-18b (-2.2(-1.5)(+1.4)) is slightly higher than the value predicted by the self-consistent model assuming solar abundance. For WASP-76b, the retrieved CO mixing ratio (-3.6(-1.6)(+1.8)) is broadly consistent with the value of solar abundance. In addition, we included the equatorial rotation velocity (upsilon(eq)) in the retrieval when analyzing the line profile broadening. The obtained upsilon(eq) is 7.0 +/- 2.9 km s(-1) for WASP-18b and 5.2(-3.0)(+2.5) km s(-1) for WASP-76b, which are consistent with the tidally locked rotational velocities.

Place, publisher, year, edition, pages
EDP SciencesEDP SCIENCES S A, 2023
Keywords
planets and satellites, atmospheres, techniques, spectroscopic, individual, WASP-18b, WASP-76b
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-501983 (URN)10.1051/0004-6361/202245371 (DOI)000964933400002 ()
Funder
Knut and Alice Wallenberg Foundation
Available from: 2023-05-22 Created: 2023-05-22 Last updated: 2024-01-15Bibliographically approved
Dorn, R. J., Bristow, P., Smoker, J. V., Rodler, F., Lavail, A., Accardo, M., . . . Wehrhahn, A. (2023). CRIRES+ on sky at the ESO Very Large Telescope: Observing the Universe at infrared wavelengths and high spectral resolution. Astronomy and Astrophysics, 671, Article ID A24.
Open this publication in new window or tab >>CRIRES+ on sky at the ESO Very Large Telescope: Observing the Universe at infrared wavelengths and high spectral resolution
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2023 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 671, article id A24Article in journal (Refereed) Published
Abstract [en]

The CRyogenic InfraRed Echelle Spectrograph (CRIRES) Upgrade project CRIRES+ extended the capabilities of CRIRES. It transformed this VLT instrument into a cross-dispersed spectrograph to increase the wavelength range that is covered simultaneously by up to a factor of ten. In addition, a new detector focal plane array of three Hawaii 2RG detectors with a 5.3 mu m cutoff wavelength replaced the existing detectors. Amongst many other improvements, a new spectropolarimetric unit was added and the calibration system has been enhanced. The instrument was installed at the VLT on Unit Telescope 3 at the beginning of 2020 and successfully commissioned and verified for science operations during 2021, partly remotely from Europe due to the COVID-19 pandemic. The instrument was subsequently offered to the community from October 2021 onwards. This article describes the performance and capabilities of the upgraded instrument and presents on sky results.

Place, publisher, year, edition, pages
EDP Sciences, 2023
Keywords
instrumentation, spectrographs, techniques, radial velocities, polarimeters, spectroscopic, adaptive optics
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-507485 (URN)10.1051/0004-6361/202245217 (DOI)000975275100001 ()
Available from: 2023-07-07 Created: 2023-07-07 Last updated: 2023-07-07Bibliographically approved
Hahlin, A., Kochukhov, O., Rains, A., Lavail, A., Hatzes, A., Piskunov, N., . . . Stempels, H. C. (2023). Determination of small-scale magnetic fields on Sun-like stars in the near-infrared using CRIRES+. Astronomy and Astrophysics, 675, Article ID A91.
Open this publication in new window or tab >>Determination of small-scale magnetic fields on Sun-like stars in the near-infrared using CRIRES+
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2023 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 675, article id A91Article in journal (Refereed) Published
Abstract [en]

Aims: We aim to characterise the small-scale magnetic fields of a sample of 16 Sun-like stars and investigate the capabilities of the newly upgraded near-infrared (NIR) instrument CRIRES+ at the Very Large Telescope in the context of small-scale magnetic field studies. Our targets also had their magnetic fields studied with optical spectra, which allowed us to compare magnetic field properties at different spatial scales on the stellar surface and to contrast small-scale magnetic field measurements at different wavelengths.

Methods: We analysed the Zeeman broadening signature for six magnetically sensitive and insensitive Fe I lines in the H-band to measure small-scale magnetic fields on the stellar surfaces of our sample. We used polarised radiative transfer modelling and non-local thermodynamic equilibrium departure coefficients in combination with Markov chain Monte Carlo sampling to determine magnetic field characteristics and non-magnetic stellar parameters. We used two different approaches to describe the small-scale magnetic fields. The first is a two-component model with a single magnetic region and a free magnetic field strength. The second model contains multiple magnetic components with fixed magnetic field strengths.

Results: We found average magnetic field strengths ranging from & SIM;0.4 kG down to < 0.1 kG. The results align closely with other results from high-resolution NIR spectrographs, such as SPIRou. It appears that the typical magnetic field strength in the magnetic region is slightly stronger than 1.3 kG, and for most stars in our sample, this strength is between 1 and 2 kG. We also found that the small-scale fields correlate with the large-scale fields and that the small-scale fields are at least ten times stronger than the large-scale fields inferred with Zeeman Doppler imaging. The two- and multi-component models produce systematically different results, as the strong fields from the multi-component model increase the obtained mean magnetic field strength. When comparing our results with the optical measurements of small-scale fields, we found a systematic offset two to three times stronger than fields in the optical results. This discrepancy cannot be explained by uncertainties in stellar parameters. Care should therefore be taken when comparing results obtained at different wavelengths until a clear cause can be established.

Place, publisher, year, edition, pages
EDP Sciences, 2023
Keywords
stars, magnetic field, solar-type, techniques, spectroscopic
National Category
Astronomy, Astrophysics and Cosmology Condensed Matter Physics
Identifiers
urn:nbn:se:uu:diva-509279 (URN)10.1051/0004-6361/202346314 (DOI)001023434900010 ()
Funder
Swedish Research Council, 2019-03548Knut and Alice Wallenberg Foundation
Available from: 2023-08-23 Created: 2023-08-23 Last updated: 2023-08-23Bibliographically approved
Projects
Participation with invited talk in HELAS workshop Interpretation of Asteroseismic Data, Wroclaw, Poland, 2008-06-22--28. [2008-01501_VR]; Uppsala UniversityMagnetic Fields: the New Cornerstone of Stellar Physics [2009-04045_VR]; Uppsala UniversityMagnetic fields: a new cornerstone of stellar physics [2010-04103_VR]; Uppsala UniversityPLATO - Spectropolarimetry [185/14 N_SNSB]; Uppsala UniversityAn insight into atmospheres and formation of exosolar planets from infrared spectroscopy [2014-05720_VR]; Uppsala UniversityStellar magnetic activity: a key factor for evolution, atmospheres and habitability of terrestrial exoplanets [2019-03548_VR]; Uppsala UniversityMagnetic fields of red dwarf stars and their impact on terrestrial exoplanets [2023-03667_VR]; Uppsala University
Organisations
Identifiers
ORCID iD: ORCID iD iconorcid.org/0000-0003-3061-4591

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