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Florén, Hans Gustav AxelORCID iD iconorcid.org/0000-0001-6994-9159
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Publications (10 of 43) Show all publications
Sicardy, B., Brandeker, A., Florén, H. G., Olofsson, G. & Kate, A. (2024). Constraints on the evolution of the Triton atmosphere from occultations: 1989-2022. Astronomy and Astrophysics, 682, Article ID L24.
Open this publication in new window or tab >>Constraints on the evolution of the Triton atmosphere from occultations: 1989-2022
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2024 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 682, article id L24Article in journal (Refereed) Published
Abstract [en]

Context. In about 2000, the south pole of Triton experienced an extreme summer solstice that occurs every ∼650 years, when the subsolar latitude reached about 50°S. Bracketing this epoch, a few occultations probed the Triton atmosphere in 1989, 1995, 1997, 2008, and 2017. A recent ground-based stellar occultation observed on 6 October 2022 provides a new measurement of the atmospheric pressure on Triton. This is presented here.

Aims. The goal is to constrain the volatile transport models (VTMs) of the Triton atmosphere. The atmosphere is basically in vapor pressure equilibrium with the nitrogen ice at its surface.

Methods. Fits to the occultation light curves yield the atmospheric pressure of Triton at the reference radius 1400 km, from which the surface pressure is deduced.

Results. The fits provide a pressure p1400 = 1.211 ± 0.039 μbar at radius 1400 km (47 km altitude), from which a surface pressure of psurf = 14.54 ± 0.47 μbar is deduced (1σ error bars). To within the error bars, this is identical to the pressure derived from the previous occultation of 5 October 2017, p1400 = 1.18 ± 0.03 μbar and psurf = 14.1 ± 0.4 μbar, respectively. Based on recent models of the volatile cycles of Triton, the overall evolution of the surface pressure over the last 30 years is consistent with N2 condensation taking place in the northern hemisphere. However, models typically predict a steady decrease in the surface pressure for the period 2005-2060, which is not confirmed by this observation. Complex surface-atmosphere interactions, such as ice albedo runaway and formation of local N2 frosts in the equatorial regions of Triton, could explain the relatively constant pressure between 2017 and 2022.

Keywords
planets and satellites: atmospheres, planets and satellites: individual: Triton
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:su:diva-228907 (URN)10.1051/0004-6361/202348756 (DOI)001178184800004 ()2-s2.0-85186740734 (Scopus ID)
Available from: 2024-05-03 Created: 2024-05-03 Last updated: 2024-05-03Bibliographically approved
Fridlund, M., Olofsson, G., Brandeker, A., Florén, H. G. & Walton, N. A. (2024). Planets observed with CHEOPS: Two super-Earths orbiting the red dwarf star TOI-776. Astronomy and Astrophysics, 684, Article ID A12.
Open this publication in new window or tab >>Planets observed with CHEOPS: Two super-Earths orbiting the red dwarf star TOI-776
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2024 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 684, article id A12Article in journal (Refereed) Published
Abstract [en]

Context. M-dwarf stars are the most common of potential exoplanet host stars in the Galaxy. It is therefore very important to understand planetary systems orbiting such stars and to determine the physical parameters of such planets with high precision. Also with the launch of the James Webb Space Telescope (JWST) the observation of atmospheric parameters of planets orbiting these stars has begun. It is therefore required to determine properties of potential targets.

Aims. Two planets around the red dwarf TOI-776 were detected by TESS. The objective of our study was to use transit observations obtained by the CHEOPS space mission to improve the current precision of the planetary radii, as well as additional radial velocity (RV) data in order to improve mass estimates of the two planets. Using these quantities, we wanted to derive the bulk densities of those planets, improving the precision in earlier results, and use this information to put them in context of other exoplanetary systems involving very low mass stars.

Methods. Utilizing new transit data from the CHEOPS satellite and its photometric telescope, we obtained very high precision planetary transit measurements. Interpretation of these provides updated planetary radii, along with other system parameters. A concurrent ESO large observing program using the high precision spectrograph HARPS has doubled the available radial velocity data. Calculating the power spectrum of a number of stellar activity indices we update the previously estimated stellar rotation period to a lower value.

Results. The CHEOPS data provide precise transit depths of 909 and 1177 ppm translating into radii of Rb = R and Rc = R, respectively. Our interpretation of the radial velocities and activity indicator time series data estimates a stellar rotation period for this early M dwarf of ~21.1 days. A further multi-dimensional Gaussian process approach confirm this new estimate. By performing a Skew-Normal (SN) fit onto the Cross Correlation Functions we extracted the RV data and the activity indicators to estimate the planetary masses, obtaining Mb = M and Mc = M.

Conclusions. We improve the precision in planetary radius for TOI-776 b and c by a factor of more than two. Our data and modelling give us parameters of both bodies consistent with mini-Neptunes, albeit with a relatively high density. The stellar activity of TOI-776 is found to have increased by a factor larger than 2 since the last set of observations.

Keywords
techniques: photometric, techniques: spectroscopic, planets and satellites: detection, planets and satellites: individual: TOI-776 b, planets and satellites: individual: TOI-776 c, stars: individual: LP 961-53
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:su:diva-228977 (URN)10.1051/0004-6361/202243838 (DOI)001198847900010 ()2-s2.0-85184520440 (Scopus ID)
Available from: 2024-05-13 Created: 2024-05-13 Last updated: 2024-05-13Bibliographically approved
Morgado, B. E., Brandeker, A., Florén, H. G., Olofsson, G. & de Wit, J. (2023). A dense ring of the trans-Neptunian object Quaoar outside its Roche limit. Nature, 614(7947), 239-243
Open this publication in new window or tab >>A dense ring of the trans-Neptunian object Quaoar outside its Roche limit
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2023 (English)In: Nature, ISSN 0028-0836, E-ISSN 1476-4687, Vol. 614, no 7947, p. 239-243Article in journal (Refereed) Published
Abstract [en]

In our efforts to characterize Quaoar’s shape and search for putative material around it, we have predicted and observed several stellar occultations by this body. Following a report from Australia of a Neptune-like ring detected during a 2021 occultation and independently suspected in 2019, we have identified secondary events in previous occultations observed between 2018 and 2020. They are consistent with a circular ring centred on the body, with two possible mirror solutions for the ring orientation. Both solutions have radii close to 4,100 km, or roughly 7.4 Quaoar radii. One solution has a ring pole that presents a large mismatch with Weywot’s orbital pole, whereas the other solution is consistent with a ring coplanar with Weywot’s orbit. This is our preferred solution, as a primordial collisional system surrounding Quaoar is expected to settle in a disc that subsequently forms both the ring and Weywot.

National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:su:diva-216054 (URN)10.1038/s41586-022-05629-6 (DOI)000941028700001 ()36755175 (PubMedID)2-s2.0-85147724719 (Scopus ID)
Available from: 2023-03-31 Created: 2023-03-31 Last updated: 2023-03-31Bibliographically approved
Ehrenreich, D., Olofsson, G., Brandeker, A., Florén, H. G. & Walton, N. A. (2023). A full transit of v2 Lupi d and the search for an exomoon in its Hill sphere with CHEOPS. Astronomy and Astrophysics, 671, Article ID A154.
Open this publication in new window or tab >>A full transit of v2 Lupi d and the search for an exomoon in its Hill sphere with CHEOPS
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2023 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 671, article id A154Article in journal (Refereed) Published
Abstract [en]

The planetary system around the naked-eye star v2 Lupi (HD 136352; TOI-2011) is composed of three exoplanets with masses of 4.7, 11.2, and 8.6 Earth masses (M). The TESS and CHEOPS missions revealed that all three planets are transiting and have radii straddling the radius gap separating volatile-rich and volatile-poor super-earths. Only a partial transit of planet d had been covered so we re-observed an inferior conjunction of the long-period 8.6 M exoplanet v2 Lup d with the CHEOPS space telescope. We confirmed its transiting nature by covering its whole 9.1 h transit for the first time. We refined the planet transit ephemeris to P = 107.1361−0.0022+0.0019 days and Tc = 2459009.7759−0.0096+0.0101 BJDTDB, improving by ~40 times on the previously reported transit timing uncertainty. This refined ephemeris will enable further follow-up of this outstanding long-period transiting planet to search for atmospheric signatures or explore the planet’s Hill sphere in search for an exomoon. In fact, the CHEOPS observations also cover the transit of a large fraction of the planet’s Hill sphere, which is as large as the Earth’s, opening the tantalising possibility of catching transiting exomoons. We conducted a search for exomoon signals in this single-epoch light curve but found no conclusive photometric signature of additional transiting bodies larger than Mars. Yet, only a sustained follow-up of v2 Lup d transits will warrant a comprehensive search for a moon around this outstanding exoplanet.

Keywords
planets and satellites: detection, planets and satellites: individual: HD 136352, planets and satellites: general
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:su:diva-220589 (URN)10.1051/0004-6361/202244790 (DOI)000982504800001 ()2-s2.0-85150788165 (Scopus ID)
Available from: 2023-08-31 Created: 2023-08-31 Last updated: 2023-08-31Bibliographically approved
Florén, H. G., Brandeker, A. & Olofsson, G. (2023). Discovery of TOI-1260d and the characterization of the multiplanet system. Monthly notices of the Royal Astronomical Society, 519(1), 1437-1451
Open this publication in new window or tab >>Discovery of TOI-1260d and the characterization of the multiplanet system
2023 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 519, no 1, p. 1437-1451Article in journal (Refereed) Published
Abstract [en]

We report the discovery of a third planet transiting the star TOI-1260, previously known to host two transiting sub-Neptune planets with orbital periods of 3.127 and 7.493 d, respectively. The nature of the third transiting planet with a 16.6-d orbit is supported by ground-based follow-up observations, including time-series photometry, high-angular resolution images, spectroscopy, and archival imagery. Precise photometric monitoring with CHEOPS allows to improve the constraints on the parameters of the system, improving our knowledge on their composition. The improved radii of TOI-1260b and TOI-1260c are 2.36±0.06R⊕2.36±0.06R⊕⁠, 2.82±0.08R⊕2.82±0.08R⊕⁠, respectively while the newly discovered third planet has a radius of 3.09±0.09R⊕3.09±0.09R⊕⁠. The radius uncertainties are in the range of 3 per cent, allowing a precise interpretation of the interior structure of the three planets. Our planet interior composition model suggests that all three planets in the TOI-1260 system contains some fraction of gas. The innermost planet TOI-1260b has most likely lost all of its primordial hydrogen-dominated envelope. Planets c and d were also likely to have experienced significant loss of atmospheric through escape, but to a lesser extent compared to planet b.

Keywords
techniques: photometric, techniques: radial velocities, planets and satellites: composition, planets and satellites: detection, planets and satellites: individual: TOI-1260b, c, d, stars: individual: TOI-1260
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:su:diva-215721 (URN)10.1093/mnras/stac3639 (DOI)000927884000010 ()
Available from: 2023-03-27 Created: 2023-03-27 Last updated: 2023-03-27Bibliographically approved
Florén, H. G., Brandeker, A. & Olofsson, G. (2023). Examining the orbital decay targets KELT-9 b, KELT-16 b, and WASP-4 b, and the transit-timing variations of HD 97658 b. Astronomy and Astrophysics, 669, Article ID A124.
Open this publication in new window or tab >>Examining the orbital decay targets KELT-9 b, KELT-16 b, and WASP-4 b, and the transit-timing variations of HD 97658 b
2023 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 669, article id A124Article in journal (Refereed) Published
Abstract [en]

Context. Tidal orbital decay is suspected to occur for hot Jupiters in particular, with the only observationally confirmed case of this being WASP-12b. By examining this effect, information on the properties of the host star can be obtained using the so-called stellar modified tidal quality factor Q*, which describes the efficiency with which the kinetic energy of the planet is dissipated within the star. This can provide information about the interior of the star.

Aims. In this study, we aim to improve constraints on the tidal decay of the KELT-9, KELT-16, and WASP-4 systems in order to find evidence for or against the presence of tidal orbital decay. With this, we want to constrain the Q* value for each star. In addition, we aim to test the existence of the transit timing variations (TTVs) in the HD 97658 system, which previously favoured a quadratic trend with increasing orbital period.

Methods. Making use of newly acquired photometric observations from CHEOPS (CHaracterising ExOplanet Satellite) and TESS (Transiting Exoplanet Survey Satellite), combined with archival transit and occultation data, we use Markov chain Monte Carlo (MCMC) algorithms to fit three models to the data, namely a constant-period model, an orbital-decay model, and an apsidal-precession model.

Results. We find that the KELT-9 system is best described by an apsidal-precession model for now, with an orbital decay trend at over 2 σ being a possible solution as well. A Keplerian orbit model with a constant orbital period provides the best fit to the transit timings of KELT-16 b because of the scatter and scale of their error bars. The WASP-4 system is best represented by an orbital decay model at a 5 σ significance, although apsidal precession cannot be ruled out with the present data. For HD 97658 b, using recently acquired transit observations, we find no conclusive evidence for a previously suspected strong quadratic trend in the data.

Keywords
planets and satellites, dynamical evolution and stability, planet-star interactions, techniques, photometric
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:su:diva-215725 (URN)10.1051/0004-6361/202244529 (DOI)000921718300001 ()2-s2.0-85147138880 (Scopus ID)
Available from: 2023-03-27 Created: 2023-03-27 Last updated: 2023-03-27Bibliographically approved
Alonso, R., Florén, H. G., Brandeker, A., Olofsson, H. & Walton, N. A. (2023). No random transits in CHEOPS observations of HD 139139. Astronomy and Astrophysics, 680, Article ID A78.
Open this publication in new window or tab >>No random transits in CHEOPS observations of HD 139139
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2023 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 680, article id A78Article in journal (Refereed) Published
Abstract [en]

Context. The star HD 139139 (a.k.a. 'the Random Transiter') is a star that exhibited enigmatic transit-like features with no apparent periodicity in K2 data. The shallow depth of the events (similar to 200 ppm - equivalent to transiting objects with radii of similar to 1.5 R-circle plus in front of a Sun-like star) and their non-periodicity constitute a challenge for the photometric follow-up of this star. Aims. The goal of this study is to confirm with independent measurements the presence of shallow, non-periodic transit-like features on this object. Methods. We performed observations with CHEOPS for a total accumulated time of 12.75 days, distributed in visits of roughly 20 h in two observing campaigns in years 2021 and 2022. The precision of the data is sufficient to detect 150 ppm features with durations longer than 1.5 h. We used the duration and times of the events seen in the K2 curve to estimate how many events should have been detected in our campaigns, under the assumption that their behaviour during the CHEOPS observations would be the same as in the K2 data of 2017. Results. We do not detect events with depths larger than 150 ppm in our data set. If the frequency, depth, and duration of the events were the same as in the K2 campaign, we estimate the probability of having missed all events due to our limited observing window would be 4.8%. Conclusions. We suggest three different scenarios to explain our results : 1) Our observing window was not long enough, and the events were missed with the estimated 4.8% probability. 2) The events recorded in the K2 observations were time critical, and the mechanism producing them was either not active in the 2021 and 2022 campaigns or created shallower events under our detectability level. 3) The enigmatic events in the K2 data are the result of an unidentified and infrequent instrumental noise in the original data set or its data treatment.

Keywords
stars: peculiar, planets and satellites: detection, techniques: photometric
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:su:diva-225832 (URN)10.1051/0004-6361/202347779 (DOI)001125994200008 ()2-s2.0-85180601746 (Scopus ID)
Available from: 2024-01-23 Created: 2024-01-23 Last updated: 2024-01-23Bibliographically approved
Florén, H. G. & Brandeker, A. (2023). The planetary system around HD 190622 (TOI-1054) Measuring the gas content of low-mass planets orbiting F-stars. Astronomy and Astrophysics, 675, Article ID A183.
Open this publication in new window or tab >>The planetary system around HD 190622 (TOI-1054) Measuring the gas content of low-mass planets orbiting F-stars
2023 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 675, article id A183Article in journal (Refereed) Published
Abstract [en]

Context. Giant planets are known to dominate the long-term stability of planetary systems due to their prevailing gravitational interactions, but they are also thought to play an important role in planet formation. Observational constraints improve our understanding of planetary formation processes such as the delivery of volatile-rich planetesimals from beyond the ice line into the inner planetary system. Additional constraints may come from studies of the atmosphere, but almost all such studies of the atmosphere investigate the detection of certain species, and abundances are not routinely quantitatively measured.

Aims. Accurate measurements of planetary bulk parameters – that is, mass and density – provide constraints on the inner structure and chemical composition of transiting planets. This information provides insight into properties such as the amounts of volatile species, which in turn can be related to formation and evolution processes.

Methods. The Transiting Exoplanet Survey Satellite (TESS) reported a planetary candidate around HD 190622 (TOI-1054), which was subsequently validated and found to merit further characterization with photometric and spectroscopic facilities. The KESPRINT collaboration used data from the High Accuracy Radial Velocity Planet Searcher (HARPS) to independently confirm the planetary candidate, securing its mass, and revealing the presence of an outer giant planet in the system. The CHEOPS consortium invested telescope time in the transiting target in order to reduce the uncertainty on the radius, improving the characterization of the planet.

Results. We present the discovery and characterization of the planetary system around HD 190622 (TOI-1054). This system hosts one transiting planet, which is smaller than Neptune (3.087-0.053+0.058REarth, 7.7 ± 1.0 MEarth) but has a similar bulk density (1.43 ± 0.21 g cm−3) and an orbital period of 16 days; and a giant planet, not known to be transiting, with a minimum mass of 227.0 ± 6.7 MEarth in an orbit with a period of 315 days.

Conclusions. Our measurements constrain the structure and composition of the transiting planet. HD 190622b has singular properties among the known population of transiting planets, which we discuss in detail. Among the sub-Neptune-sized planets known today, this planet stands out because of its large gas content.

Keywords
planetary systems, planets and satellites: detection
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:su:diva-221688 (URN)10.1051/0004-6361/202245774 (DOI)001049599200008 ()2-s2.0-85166229075 (Scopus ID)
Available from: 2023-09-27 Created: 2023-09-27 Last updated: 2023-09-27Bibliographically approved
Bonfanti, A., Florén, H. G., Brandeker, A., Olofsson, G. & Walton, N. A. (2023). TOI-1055 b: Neptunian planet characterised with HARPS, TESS, and CHEOPS. Astronomy and Astrophysics, 671, Article ID L8.
Open this publication in new window or tab >>TOI-1055 b: Neptunian planet characterised with HARPS, TESS, and CHEOPS
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2023 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 671, article id L8Article in journal (Refereed) Published
Abstract [en]

Context. TOI-1055 is a Sun-like star known to host a transiting Neptune-sized planet on a 17.5-day orbit (TOI-1055 b). Radial velocity (RV) analyses carried out by two independent groups using nearly the same set of HARPS spectra have provided measurements of planetary masses that differ by ∼2σ.

Aims. Our aim in this work is to solve the inconsistency in the published planetary masses by significantly extending the set of HARPS RV measurements and employing a new analysis tool that is able to account and correct for stellar activity. Our further aim was to improve the precision on measurements of the planetary radius by observing two transits of the planet with the CHEOPS space telescope.

Methods. We fit a skew normal function to each cross correlation function extracted from the HARPS spectra to obtain RV measurements and hyperparameters to be used for the detrending. We evaluated the correlation changes of the hyperparameters along the RV time series using the breakpoint technique. We performed a joint photometric and RV analysis using a Markov chain Monte Carlo scheme to simultaneously detrend the light curves and the RV time series.

Results. We firmly detected the Keplerian signal of TOI-1055 b, deriving a planetary mass of Mb = 20.4−2.5+2.6 M (∼12%). This value is in agreement with one of the two estimates in the literature, but it is significantly more precise. Thanks to the TESS transit light curves combined with exquisite CHEOPS photometry, we also derived a planetary radius of Rb = 3.490−0.064+0.070 R (∼1.9%). Our mass and radius measurements imply a mean density of ρb = 2.65−0.35+0.37 g cm−3 (∼14%). We further inferred the planetary structure and found that TOI-1055 b is very likely to host a substantial gas envelope with a mass of 0.41−0.20+0.34 M and a thickness of 1.05−0.29+0.30 R.

Conclusions. Our RV extraction combined with the breakpoint technique has played a key role in the optimal removal of stellar activity from the HARPS time series, enabling us to solve the tension in the planetary mass values published so far for TOI-1055 b.

Keywords
techniques: radial velocities, techniques: photometric, planets and satellites: fundamental parameters, stars: fundamental parameters
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:su:diva-220590 (URN)10.1051/0004-6361/202245607 (DOI)000982354400009 ()2-s2.0-85149928701 (Scopus ID)
Available from: 2023-08-31 Created: 2023-08-31 Last updated: 2023-08-31Bibliographically approved
Florén, H. G., Brandeker, A. & Olofsson, G. (2022). A CHEOPS-enhanced view of the HD 3167 system. Astronomy and Astrophysics, 668, Article ID A31.
Open this publication in new window or tab >>A CHEOPS-enhanced view of the HD 3167 system
2022 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 668, article id A31Article in journal (Refereed) Published
Abstract [en]

Much remains to be understood about the nature of exoplanets smaller than Neptune, most of which have been discovered in compact multi-planet systems. With its inner ultra-short period planet b aligned with the star and two larger outer planets d-c on polar orbits, the multi-planet system HD 3167 features a peculiar architecture and offers the possibility to investigate both dynamical and atmospheric evolution processes. To this purpose we combined multiple datasets of transit photometry and radial velocimetry (RV) to revise the properties of the system and inform models of its planets. This effort was spearheaded by CHEOPS observations of HD 3167b, which appear inconsistent with a purely rocky composition despite its extreme irradiation. Overall the precision on the planetary orbital periods are improved by an order of magnitude, and the uncertainties on the densities of the transiting planets b and c are decreased by a factor of 3. Internal structure and atmospheric simulations draw a contrasting picture between HD 3167d, likely a rocky super-Earth that lost its atmosphere through photo-evaporation, and HD 3167c, a mini-Neptune that kept a substantial primordial gaseous envelope. We detect a fourth, more massive planet on a larger orbit, likely coplanar with HD 3167d-c. Dynamical simulations indeed show that the outer planetary system d-c-e was tilted, as a whole, early in the system history, when HD 3167b was still dominated by the star influence and maintained its aligned orbit. RV data and direct imaging rule out that the companion that could be responsible for the present-day architecture is still bound to the HD 3167 system. Similar global studies of multi-planet systems will tell how many share the peculiar properties of the HD 3167 system, which remains a target of choice for follow-up observations and simulations.

Keywords
planets and satellites: individual: HD 3167, planets and satellites: dynamical evolution and stability, planets and satellites: physical evolution, techniques: photometric, techniques: radial velocities, planet-star interactions
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:su:diva-215722 (URN)10.1051/0004-6361/202243778 (DOI)000934061500006 ()2-s2.0-85145347243 (Scopus ID)
Available from: 2023-03-27 Created: 2023-03-27 Last updated: 2023-03-27Bibliographically approved
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ORCID iD: ORCID iD iconorcid.org/0000-0001-6994-9159

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