Logo: to the web site of Uppsala University

uu.sePublications from Uppsala University
Change search
Link to record
Permanent link

Direct link
Alternative names
Publications (10 of 131) Show all publications
Edberg, N. J. T., Eriksson, A. I., Vigren, E., Nilsson, H., Gunell, H., Götz, C., . . . De Keyser, J. (2024). Scale size of cometary bow shocks. Astronomy and Astrophysics, 682, Article ID A51.
Open this publication in new window or tab >>Scale size of cometary bow shocks
Show others...
2024 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 682, article id A51Article in journal (Refereed) Published
Abstract [en]

Context. In past decades, several spacecraft have visited comets to investigate their plasma environments. In the coming years, Comet Interceptor will make yet another attempt. This time, the target comet and its outgassing activity are unknown and may not be known before the spacecraft has been launched into its parking orbit, where it will await a possible interception. If the approximate outgassing rate can be estimated remotely when a target has been identified, it is desirable to also be able to estimate the scale size of the plasma environment, defined here as the region bound by the bow shock.

Aims. This study aims to combine previous measurements and simulations of cometary bow shock locations to gain a better understanding of how the scale size of cometary plasma environments varies. We compare these data with models of the bow shock size, and we furthermore provide an outgassing rate-dependent shape model of the bow shock. We then use this to predict a range of times and cometocentric distances for the crossing of the bow shock by Comet Interceptor, together with expected plasma density measurements along the spacecraft track.

Methods. We used data of the location of cometary bow shocks from previous spacecraft missions, together with simulation results from previously published studies. We compared these results with an existing model of the bow shock stand-off distance and expand on this to provide a shape model of cometary bow shocks. The model in particular includes the cometary outgassing rate, but also upstream solar wind conditions, ionisation rates, and the neutral flow velocity.

Results. The agreement between the gas-dynamic model and the data and simulation results is good in terms of the stand-off distance of the bow shock as a function of the outgassing rate. For outgassing rates in the range of 1027–1031–s-1, the scale size of cometary bow shocks can vary by four orders of magnitude, from about 102 km to 106 km, for an ionisation rate, flow velocity, and upstream solar wind conditions typical of those at 1 AU. The proposed bow shock shape model shows that a comet plasma environment can range in scale size from the plasma environment of Mars to about half of that of Saturn.

Conclusions. The model-data agreement allows for the planning of upcoming spacecraft comet encounters, such as that of Comet Interceptor, when a target has been identified and its outgassing rate is determined. We conclude that the time a spacecraft can spend within the plasma environment during a flyby can range from minutes to days, depending on the comet that is visited and on the flyby speed. However, to capture most of the comet plasma environment, including pick-up ions and upstream plasma waves, and to ensure the highest possible scientific return, measurements should still start well upstream of the expected bow shock location. From the plasma perspective, the selected target should preferably be an active comet with the lowest possible flyby velocity.

Place, publisher, year, edition, pages
EDP Sciences, 2024
Keywords
comets: general, plasmas
National Category
Fusion, Plasma and Space Physics Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-525518 (URN)10.1051/0004-6361/202346566 (DOI)001163661400003 ()
Funder
Swedish Research Council, 2020-03962
Available from: 2024-03-25 Created: 2024-03-25 Last updated: 2024-03-25Bibliographically approved
Jones, G. H., Snodgrass, C., Tubiana, C., Kuppers, M., Kawakita, H., Lara, L. M., . . . Ji, H. (2024). The Comet Interceptor Mission. Space Science Reviews, 220(1), Article ID 9.
Open this publication in new window or tab >>The Comet Interceptor Mission
Show others...
2024 (English)In: Space Science Reviews, ISSN 0038-6308, E-ISSN 1572-9672, Vol. 220, no 1, article id 9Article, review/survey (Refereed) Published
Abstract [en]

Here we describe the novel, multi-point Comet Interceptor mission. It is dedicated to the exploration of a little-processed long-period comet, possibly entering the inner Solar System for the first time, or to encounter an interstellar object originating at another star. The objectives of the mission are to address the following questions: What are the surface composition, shape, morphology, and structure of the target object? What is the composition of the gas and dust in the coma, its connection to the nucleus, and the nature of its interaction with the solar wind? The mission was proposed to the European Space Agency in 2018, and formally adopted by the agency in June 2022, for launch in 2029 together with the Ariel mission. Comet Interceptor will take advantage of the opportunity presented by ESA’s F-Class call for fast, flexible, low-cost missions to which it was proposed. The call required a launch to a halo orbit around the Sun-Earth L2 point. The mission can take advantage of this placement to wait for the discovery of a suitable comet reachable with its minimum ΔV capability of 600 ms−1. Comet Interceptor will be unique in encountering and studying, at a nominal closest approach distance of 1000 km, a comet that represents a near-pristine sample of material from the formation of the Solar System. It will also add a capability that no previous cometary mission has had, which is to deploy two sub-probes – B1, provided by the Japanese space agency, JAXA, and B2 – that will follow different trajectories through the coma. While the main probe passes at a nominal 1000 km distance, probes B1 and B2 will follow different chords through the coma at distances of 850 km and 400 km, respectively. The result will be unique, simultaneous, spatially resolved information of the 3-dimensional properties of the target comet and its interaction with the space environment. We present the mission’s science background leading to these objectives, as well as an overview of the scientific instruments, mission design, and schedule.

Place, publisher, year, edition, pages
Springer, 2024
Keywords
Comets, Spacecraft, Instruments - spaceborne and space research
National Category
Astronomy, Astrophysics and Cosmology Fusion, Plasma and Space Physics Aerospace Engineering
Identifiers
urn:nbn:se:uu:diva-528346 (URN)10.1007/s11214-023-01035-0 (DOI)001194889900001 ()38282745 (PubMedID)
Funder
Swedish National Space Board, 108/18Swedish National Space Board, 2021-00047EU, Horizon 2020, 802699EU, Horizon 2020, 101079231The European Space Agency (ESA), 4000136673/21/NL/IB/igThe European Space Agency (ESA), 3-17164/21/NL/GP/pbeAcademy of Finland, 1345115Academy of Finland, 1336546Academy of Finland, 325805Academy of Finland, 335595EU, Horizon Europe, 10051045
Available from: 2024-05-20 Created: 2024-05-20 Last updated: 2024-05-27Bibliographically approved
Vigren, E., Eriksson, A., Edberg, N. J. T. & Snodgrass, C. (2023). A potential aid in the target selection for the comet interceptor mission. Planetary and Space Science, 237, Article ID 105765.
Open this publication in new window or tab >>A potential aid in the target selection for the comet interceptor mission
2023 (English)In: Planetary and Space Science, ISSN 0032-0633, E-ISSN 1873-5088, Vol. 237, article id 105765Article in journal (Refereed) Published
Abstract [en]

The upcoming Comet Interceptor mission involves a parking phase around the Sun-Earth L2 point before transferring to intercept the orbit of a long period comet, interstellar object or a back-up target in the form of a short-period comet. The target is not certain to be known before the launch in 2029. During the parking phase there may thus arise a scenario wherein a decision needs to be taken of whether to go for a particular comet or whether to discard that option in the hope that a better target will appear within a reasonable time frame later on. We present an expectation value-based formalism that could aid in the associated decision making provided that outlined requirements for its implementation exist.

Place, publisher, year, edition, pages
Elsevier, 2023
Keywords
Comets, Solar system, Probability theory
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-514901 (URN)10.1016/j.pss.2023.105765 (DOI)001071302000001 ()
Funder
Swedish National Space Board, 202100047
Available from: 2023-10-31 Created: 2023-10-31 Last updated: 2023-10-31Bibliographically approved
Andrews, D. J., Stergiopoulou, K., Andersson, L., Eriksson, A., Ergun, R. & Pilinski, M. (2023). Electron densities and temperatures in the Martian ionosphere: MAVEN LPW observations of control by crustal fields. Journal of Geophysical Research - Space Physics, 128(3), Article ID e2022JA031027.
Open this publication in new window or tab >>Electron densities and temperatures in the Martian ionosphere: MAVEN LPW observations of control by crustal fields
Show others...
2023 (English)In: Journal of Geophysical Research - Space Physics, ISSN 2169-9380, E-ISSN 2169-9402, Vol. 128, no 3, article id e2022JA031027Article in journal (Refereed) Published
Abstract [en]

Mars Express and Mars Atmosphere and Volatile Evolution (MAVEN) observations have demonstrated the influence of Mars's spatially variable crustal magnetic fields upon the configuration of the plasma in the ionosphere. This influence furthermore leads to variations in ionospheric escape, conceivably in part through the modification of the plasma density and electron temperature in the upper ionosphere. In this study, we examine MAVEN Langmuir Probe and Waves data, finding a clear correspondence between the structure of the crustal fields and both the measured electron temperatures and densities, by first constructing an "average " profile from which departures can be quantified. Electron temperatures are shown to be lower in regions of strong crustal fields over a wide altitude range. We extend previous analyses to cover the nightside ionosphere, finding the same effects present to a lesser degree, in contrast to previous studies where the opposite relationship was found between densities and crustal fields. We further determine the altitude range over which this coupling between both plasma density (and temperature) and crustal fields is effective and use measurements made by MAVEN in the solar wind to explore the dependence of this crustal field control on the coupling to the solar wind and the interplanetary magnetic field (IMF). Based on this, there is some suggestion that variations in the solar wind dynamic pressure are associated with modulation of the effects of the crustal fields on plasma density, whereas the strength of the IMF modulates the crustal fields effects on both electron densities and temperatures.

Place, publisher, year, edition, pages
American Geophysical Union (AGU), 2023
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-481217 (URN)10.1029/2022JA031027 (DOI)000934590000001 ()
Funder
Swedish National Space Board, DNR 156/16
Available from: 2022-08-06 Created: 2022-08-06 Last updated: 2023-03-13Bibliographically approved
Vigren, E., Dreyer, J., Eriksson, A. I., Johansson, F. L., Morooka, M. & Wahlund, J.-E. (2022). Empirical Photochemical Modeling of Saturn's Ionization Balance Including Grain Charging. The Planetary Science Journal, 3(2), Article ID 49.
Open this publication in new window or tab >>Empirical Photochemical Modeling of Saturn's Ionization Balance Including Grain Charging
Show others...
2022 (English)In: The Planetary Science Journal, E-ISSN 2632-3338, Vol. 3, no 2, article id 49Article in journal (Refereed) Published
Abstract [en]

We present a semianalytical photochemical model of Saturn's near-equatorial ionosphere and adapt it to two regions (similar to 2200 and similar to 1700 km above the 1 bar level) probed during the inbound portion of Cassini's orbit 292 (2017 September 9). The model uses as input the measured concentrations of molecular hydrogen, hydrogen ion species, and free electrons, as well as the measured electron temperature. The output includes upper limits, or constraints, on the mixing ratios of two families of molecules, on ion concentrations, and on the attachment rates of electrons and ions onto dust grains. The model suggests mixing ratios of the two molecular families that, particularly near similar to 1700 km, differ notably from what independent measurements by the Ion Neutral Mass Spectrometer suggest. Possibly connected to this, the model suggests an electron-depleted plasma with a level of electron depletion of around 50%. This is in qualitative agreement with interpretations of Radio Plasma Wave Science/Langmuir Probe measurements, but an additional conundrum arises in the fact that a coherent photochemical equilibrium scenario then relies on a dust component with typical grain radii smaller than 3 angstrom.

Place, publisher, year, edition, pages
Institute of Physics (IOP), 2022
National Category
Fusion, Plasma and Space Physics
Identifiers
urn:nbn:se:uu:diva-495353 (URN)10.3847/PSJ/ac4eee (DOI)000911845800001 ()
Funder
Swedish National Space Board
Available from: 2023-01-30 Created: 2023-01-30 Last updated: 2023-10-03Bibliographically approved
Johansson, F., Vigren, E., Waite, J. H., Miller, K., Eriksson, A., Edberg, N. J. T. & Dreyer, J. (2022). Implications from secondary emission from neutral impact on Cassini plasma and dust measurements. Monthly notices of the Royal Astronomical Society, 515(2), 2340-2350
Open this publication in new window or tab >>Implications from secondary emission from neutral impact on Cassini plasma and dust measurements
Show others...
2022 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 515, no 2, p. 2340-2350Article in journal (Refereed) Published
Abstract [en]

We investigate the role of secondary electron and ion emission from impact of gas molecules on the Cassini Langmuir probe (RPWS-LP or LP) measurements in the ionosphere of Saturn. We add a model of the emission currents, based on laboratory measurements and data from comet 1P/Halley, to the equations used to derive plasma parameters from LP bias voltage sweeps. Reanalysing several hundred sweeps from the Cassini Grand Finale orbits, we find reasonable explanations for three open conundrums from previous LP studies of the Saturn ionosphere. We find an explanation for the observed positive charging of the Cassini spacecraft, the possibly overestimated ionospheric electron temperatures, and the excess ion current reported. For the sweeps analysed in detail, we do not find (indirect or direct) evidence of dust having a significant charge-carrying role in Saturn's ionosphere. We also produce an estimate of H2O number density from the last six revolutions of Cassini through Saturn's ionosphere in greater detail than reported by the Ion and Neutral Mass Spectrometer. Our analysis reveals an ionosphere that is highly structured in latitude across all six final revolutions, with mixing ratios varying with two orders of magnitude in latitude and one order of magnitude between revolutions and altitude. The result is generally consistent with an empirical photochemistry model balancing the production of H+ ions with the H+ loss through charge transfer with e.g. H2O, CH4, and CO2, for which water vapour appears as the likeliest dominant source of the signal in terms of yield and concentration.

Place, publisher, year, edition, pages
Oxford University Press (OUP), 2022
Keywords
planets and satellites: atmospheres, plasmas, space vehicles: instruments, methods: data analysis, methods: observational
National Category
Fusion, Plasma and Space Physics
Identifiers
urn:nbn:se:uu:diva-482038 (URN)10.1093/mnras/stac1856 (DOI)000834368400005 ()
Funder
Swedish National Space Board, 143/18
Available from: 2022-08-19 Created: 2022-08-19 Last updated: 2022-08-19Bibliographically approved
Odelstad, E., Karlsson, T., Eriksson, A., Bergman, S. & Wieser, G. S. (2022). Ion-Ion Cross-Field Instability of Lower Hybrid Waves in the Inner Coma of Comet 67P. Journal of Geophysical Research - Space Physics, 127(9), Article ID e2022JA030535.
Open this publication in new window or tab >>Ion-Ion Cross-Field Instability of Lower Hybrid Waves in the Inner Coma of Comet 67P
Show others...
2022 (English)In: Journal of Geophysical Research - Space Physics, ISSN 2169-9380, E-ISSN 2169-9402, Vol. 127, no 9, article id e2022JA030535Article in journal (Refereed) Published
Abstract [en]

We show that an ion-ion cross-field streaming instability between cold newborn cometary ions and heated heavy ions that were picked up upstream is likely a contributing source of observed lower hybrid (LH) waves in the inner coma of comet 67P/Churyumov-Gerasimenko. Electric field oscillations in the LH frequency range are common here, and have previously been attributed mainly to the lower-hybrid drift instability, driven by gradients associated with observed local density fluctuations. However, the observed wave activity is not confined to such gradients, nor is it always strongest there. Thus, other instabilities are likely needed as well to explain the observed wave activity. Several previous works have shown the existence of multiple populations of cometary ions in the inner coma of 67P, distinguished by differences in mass, energy and/or flow direction. We here examine two selected time intervals in October and November 2015, with substantial wave activity in the LH frequency range, where we identify two distinct cometary ion populations: a bulk population of locally produced, predominantly radially outflowing ions, and a more tenuous population picked up further upstream and accelerated back toward the comet by the solar wind electric field. These two populations exhibit strong relative drifts (similar to 20 km/s, or about five times the pickup ion thermal velocity), and we perform an electrostatic dispersion analysis showing that conditions should be favorable for LH wave generation through the ion-ion cross-field instability.

Place, publisher, year, edition, pages
American Geophysical Union (AGU)American Geophysical Union (AGU), 2022
Keywords
lower hybrid waves, ion-ion cross-field instability, comets, plasma, pick-up ions, electric fields
National Category
Fusion, Plasma and Space Physics
Identifiers
urn:nbn:se:uu:diva-486107 (URN)10.1029/2022JA030535 (DOI)000856055300001 ()
Funder
Swedish National Space Board, 109/12Swedish National Space Board, 108/12Swedish National Space Board, 91/17Swedish National Space Board, 127/17Swedish Research Council, 2017-0380
Available from: 2022-10-03 Created: 2022-10-03 Last updated: 2024-01-15Bibliographically approved
Goldstein, R., Burch, J. L., Llera, K., Altwegg, K., Rubin, M., Eriksson, A. & Nilsson, H. (2022). Observations of Modulation of Ion Flux in the Coma of Comet 67P/Churyumov-Gerasimenko. Geophysical Research Letters, 49(11), Article ID e2022GL098042.
Open this publication in new window or tab >>Observations of Modulation of Ion Flux in the Coma of Comet 67P/Churyumov-Gerasimenko
Show others...
2022 (English)In: Geophysical Research Letters, ISSN 0094-8276, E-ISSN 1944-8007, Vol. 49, no 11, article id e2022GL098042Article in journal (Refereed) Published
Abstract [en]

On 6-8 June 2015, the Ion and Electron Sensor on board Rosetta observed keV-range water-group pickup ions arriving from the solar direction. Based on magnetic field intensification and variations, the appearance of the ions was likely to have been caused by a coronal mass ejection. During the 3-day period when Rosetta was 200 km from the comet, peak ion energy/charge (E/q) varied over a range from 50 eV to 1 keV in concert with neutral gas density variations caused by the rotation of the comet and its variable solar illumination. Thermal ion densities showed the same variations. The neutral density variations provided a unique opportunity to observe the repeated slowing of the solar wind by mass loading caused by charge exchange between energetic water-group ions and thermal water-group molecules. Such solar wind slowing was observed previously only by flyby missions that provided single events.

Place, publisher, year, edition, pages
American Geophysical Union (AGU)AMER GEOPHYSICAL UNION, 2022
Keywords
comets, plasma, ions, charge exchange
National Category
Fusion, Plasma and Space Physics Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-477775 (URN)10.1029/2022GL098042 (DOI)000806216800001 ()
Funder
Swedish National Space Board
Available from: 2022-06-20 Created: 2022-06-20 Last updated: 2024-01-15Bibliographically approved
Edberg, N. J. T., Johansson, F. L., Eriksson, A. I., Vigren, E., Henri, P. & De Keyser, J. (2022). Radial distribution of plasma at comet 67P: Implications for cometary flyby missions. Astronomy and Astrophysics, 663, Article ID A42.
Open this publication in new window or tab >>Radial distribution of plasma at comet 67P: Implications for cometary flyby missions
Show others...
2022 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 663, article id A42Article in journal (Refereed) Published
Abstract [en]

Context. The Rosetta spacecraft followed comet 67P/Churyumov-Gerasimenko (67P) for more than two years at a slow walking pace (similar to 1 m s(-1)) within 1500 km from the nucleus. During one of the radial movements of the spacecraft in the early phase of the mission, the radial distribution of the plasma density could be estimated, and the ionospheric density was found to be inversely proportional to the cometocentric distance r from the nucleus (a 1/r distribution). Aims. This study aims to further characterise the radial distribution of plasma around 67P throughout the mission and to expand on the initial results. We also aim to investigate how a 1/r distribution would be observed during a flyby with a fast (similar to 10's km s(-1)) spacecraft, such as the upcoming Comet Interceptor mission, when there is also an asymmetry introduced to the outgassing over the comet surface. Methods. To determine the radial distribution of the plasma, we used data from the Langmuir probe and Mutual Impedance instruments from the Rosetta Plasma Consortium during six intervals throughout the mission, for which the motion of Rosetta was approximately radial with respect to the comet. We then simulated what distribution a fast flyby mission would actually observe during its passage through a coma when there is a 1/r plasma density distribution as well as a sinusoidal variation with a phase angle (and then a sawtooth variation) multiplied to the outgassing rate. Results. The plasma density around comet 67P is found to roughly follow a 1/r dependence, although significant deviations occur in some intervals. If we normalise all data to a common outgassing rate (or heliocentric distance) and combine the intervals to a radial range of 10-1500 km, we find a 1/r(1.19) average distribution. The simulated observed density from a fast spacecraft flying through a coma with a 1/r distribution and an asymmetric outgassing can, in fact, appear anywhere in the range from a 1/r distribution to a 1/r(2) distribution, or even slightly outside of this range. Conclusions. The plasma density is distributed in such a way that it approximately decreases in a manner that is inversely proportional to the cometocentric distance. This is to be expected from the photoionisation of a collision-less, expanding neutral gas at a constant ionisation rate and expansion speed. The deviation from a pure 1/r distribution is in many cases caused by asymmetric outgassing over the surface, additional ionisation sources being present, electric fields accelerating plasma, and changing upstream solar wind conditions. A fast flyby mission can observe a radial distribution that deviates significantly from a 1/r trend if the outgassing is not symmetric over the surface. The altitude profile that will be observed depends very much on the level of outgassing asymmetry, the flyby velocity, the comet rotation rate, and the rotation phase. It is therefore essential to include data from both the inbound and outbound legs, as well as to compare plasma density to neutral density to get a more complete understanding of the radial distribution of the plasma.

Place, publisher, year, edition, pages
EDP Sciences, 2022
Keywords
plasmas, comets: general
National Category
Fusion, Plasma and Space Physics Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-481382 (URN)10.1051/0004-6361/202243776 (DOI)000822878100004 ()
Funder
Swedish National Space Board
Available from: 2022-08-11 Created: 2022-08-11 Last updated: 2022-08-11Bibliographically approved
Goetz, C., Behar, E., Beth, A., Bodewits, D., Bromley, S., Burch, J., . . . Volwerk, M. (2022). The Plasma Environment of Comet 67P/Churyumov-Gerasimenko. Space Science Reviews, 218(8), Article ID 65.
Open this publication in new window or tab >>The Plasma Environment of Comet 67P/Churyumov-Gerasimenko
Show others...
2022 (English)In: Space Science Reviews, ISSN 0038-6308, E-ISSN 1572-9672, Vol. 218, no 8, article id 65Article, review/survey (Refereed) Published
Abstract [en]

The environment of a comet is a fascinating and unique laboratory to study plasma processes and the formation of structures such as shocks and discontinuities from electron scales to ion scales and above. The European Space Agency's Rosetta mission collected data for more than two years, from the rendezvous with comet 67P/Churyumov-Gerasimenko in August 2014 until the final touch-down of the spacecraft end of September 2016. This escort phase spanned a large arc of the comet's orbit around the Sun, including its perihelion and corresponding to heliocentric distances between 3.8 AU and 1.24 AU. The length of the active mission together with this span in heliocentric and cometocentric distances make the Rosetta data set unique and much richer than sets obtained with previous cometary probes. Here, we review the results from the Rosetta mission that pertain to the plasma environment. We detail all known sources and losses of the plasma and typical processes within it. The findings from in-situ plasma measurements are complemented by remote observations of emissions from the plasma. Overviews of the methods and instruments used in the study are given as well as a short review of the Rosetta mission. The long duration of the Rosetta mission provides the opportunity to better understand how the importance of these processes changes depending on parameters like the outgassing rate and the solar wind conditions. We discuss how the shape and existence of large scale structures depend on these parameters and how the plasma within different regions of the plasma environment can be characterised. We end with a non-exhaustive list of still open questions, as well as suggestions on how to answer them in the future.

Place, publisher, year, edition, pages
Springer, 2022
National Category
Fusion, Plasma and Space Physics Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-489334 (URN)10.1007/s11214-022-00931-1 (DOI)000881719500001 ()36397966 (PubMedID)
Funder
Swedish National Space Board, 108/18
Available from: 2023-01-13 Created: 2023-01-13 Last updated: 2023-02-09Bibliographically approved
Organisations
Identifiers
ORCID iD: ORCID iD iconorcid.org/0000-0003-2926-6761

Search in DiVA

Show all publications