ODAA1
Hundreds of regular observers are sharing their work providing very valuable data to professional astronomers. This is very valuable at a time when professional astronomers face increasing competition accessing observational resources. Additionally, networks of amateur observers can react at very short notice when triggered by a new event occurring on a solar system object requiring observations, or can contribute to a global observation campaign along with professional telescopes.
Moreover, some experienced amateur astronomers use advanced methods for analysing their data meeting the requirements of professional researchers, thereby facilitating regular and close collaboration with professionals. Often this leads to publication of results in peer-reviewed scientific journals. Examples include planetary meteorology of Jupiter, Saturn, Neptune or Venus; meteoroid or bolide impacts on Jupiter; asteroid studies, cometary or exoplanet research.
Space missions also sollicitate amateur astronomers support. For example, to understand the atmospheric dynamics of the planet at the time of Juno flybys, NASA collaborates with amateur astronomers observing the Giant Planet. It showcases an exciting opportunity for amateurs to provide an unique dataset that is used to plan the high-resolution observations from JunoCam and that advances our knowledge of the Giant planet Jupiter. Contribution of amateurs range from their own images to Junocam images processing and support on selecting by vote the feature to be observed during the flybys. Other probes like Ariel or Lucy sollicitate amateur astronomers observation to support exoplanets and small bodies science.
This session will showcase results from amateur astronomers, working either by themselves or in collaboration with members of the professional community. In addition, members from both communities will be invited to share their experiences of pro-am partnerships and offer suggestions on how these should evolve in the future.
Session assets
Introduction
The extended portion of NASA’s Juno mission began on 1 August 2021 and will continue through September 2025, after which the mission is not expected to continue providing useful observations, due to a combination of fuel exhaustion and radiation damage. In the meantime, the extended mission is successfully expanding Juno’s science goals beyond those of the prime mission, as noted previously by Orton et al. (2021, 2022, 2023). Atmospheric studies will continue to be among Juno’s science goals and an area in which the world-wide community of Jupiter observers can provide significant contextual support. Juno’s remote-sensing observations will take advantage of the migration of its closest approaches (“perijoves” or PJs) toward increasingly northern latitudes. The observations include close-ups of the circumpolar cyclones and semi-chaotic cyclones known as “folded filamentary regions”. A series of radio occultations are providing vertical profiles of electron density and the neutral-atmospheric temperature over several atmospheric regions. The mission can also characterize the variability of lightning on Jupiter’s night side.
Physical Details of the Mission
The sequence of orbits and key investigations of the primary and extended missions are shown in Figure 1. We note that on PJ34, the orbital period was reduced from 53 days to 43-44 days. It was further reduced on PJ45 to 38 days and reduced again on PJ57 to ~33 days. Some characteristics of perijoves of the extended mission are shown in Table 1. We caution that while the day of year for the perijoves is reasonably fixed, the exact times may change.
Role of Amateur Astronomers
We’ve noted at previous EPSC and EPSC-DPS meetings how the amateur community can contribute to the Juno mission via their collective world-wide 24/7 coverage of Jupiter. This applies also to the cadre of professional astronomers supporting the Juno mission and its reconnaissance of the Jupiter system over a broad spectral range. For example, this community have provided the context of different regions over which Juno’s Microwave Radiometer (MWR) has sensed plumes and “hot spots” (Fletcher et al. 2020). They have also alerted observers to strong interactions between the Great Red Spot and smaller anticyclones (Sanchez-Lavega et al. 2021) and the occurrence and evolution of prominent and unusual vortices, such as “Clyde’s spot” (Hueso et al. 2022). More recently, observations were made with the NASA Infrared Telescope Facility (IRTF) that showed slow-moving bright patches in the Equatorial Zone (EZ) that were observed more continuously among the amateur community with 890-nm (“methane”) filters. The continued tracking of outbreaks in the southern part of the North Equatorial Belt (NEB) also greatly informed the Juno team and supporting astronomers regarding the systematic longitudinal distribution of outbreaks and the range of atmospheric features they generate. A perijove-by-perijove summary of Juno-supporting observations – past, current and planned - is available at the following web site: https://www.missionjuno.swri.edu/planned-observations.
We emphasize that after PJ50, Juno’s perijoves migrated to the nightside. From now through the end of the mission, images from this community will be extremely useful to provide a context for several investigations. One of these will be high on JunoCam’s agenda during this part of the mission: searches for lightning. But similar contextual information will be sought for measurements of thermal emission from the JIRAM instrument’s high-resolution maps of 5-µm emission, as well as the MWR measurements of thermal emission from the deep atmosphere. Although the highest spatial resolution from these instruments will include high northern latitudes (see Table 1) that are not well resolved by small telescopes, measurements of mid-northern latitudes will continue to be made in the absence of close-up JunoCam images. The JunoCam images will not be able to provide a visual context, except from a distance with worse spatial resolution than is possible from the amateur community. Besides the mid-northern latitudes, observations from the amateur community will also provide the visible-wavelength context for anticipated continuation of JIRAM’s 5-µm maps of much of the southern hemisphere.
Some of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004).
References
Fletcher et al. 2020. J. Geophys. Res. 125, 306399.
Hueso et al. 2022. Icarus 380,114994
Orton et al. 2021. EPSC2021-58. doi: 10.5194/epsc02921-58.
Orton et al. 2022. EPSC2022-769. doi: 10.5194/epsc2022-769.
Orton et al. 2023. DPS. id. 115.01. Bull. Amer. Astron. Soc. 55, e-id 2023n8i115p01.
Sanchez-Lavega et al. 2021. J. Geophys. Res. 126, e006686.
Figure 1. Progression of Juno orbits viewed from above Jupiter’s north pole with respect to local time of day. “PJ” designates a “perijove”, the closest approach to Jupiter on each numbered orbit. Following a Ganymede flyby on PJ34 (green orbit), the orbital period decreased from 53 days to 43-44 days (green + blue orbits). The “Great Blue Spot” (blue) orbits map an isolated patch of intense magnetic field. Following a close Europa flyby on PJ45 (aqua orbit), the period decreased to 38 days (orange orbits). Following close flybys of Io on PJ57 and PJ58 (black orbits) the period decreased to 33 days (red orbits). In reflected sunlight, Jupiter mostly appears as a crescent at perijoves following PJ58.
Figure 2. Latitudes and longitudes to be measured by the 20 radio occultations of the Juno spacecraft between PJ52 and PJ77. Locations of ingress lie largely in the northern hemisphere - locations of egress in the southern hemisphere. Locations of the Galileo Probe and Voyager-1 radio occultations are also shown for reference.
Table 1. Current estimates of perijove properties for the remainder of Juno’s extended mission: PJ64-PJ76. Information for previous perijoves and a summary of proposed, planned and executed observations at large telescopes is listed in: https://www.missionjuno.swri.edu/planned-observations.
How to cite: Orton, G., Rogers, J., Momary, T., Brueshaber, S., Hansen, C., Bolton, S., and Fletcher, L.: The Juno Extended Mission: A Final Call for Continued Support from Amateur Observers, Europlanet Science Congress 2024, Berlin, Germany, 8–13 Sep 2024, EPSC2024-134, https://doi.org/10.5194/epsc2024-134, 2024.
Our team is part of the Italian non-profit association AstronomiAmo, which aims at disseminating astronomy and promoting respect for the environment. The All-Sky TRacking, ALerts and Environment (ASTRALE) project merges both purposes, providing a beautiful view of the night sky, an automatic detection of meteors and an evaluation of the air quality index.
Specifically, ASTRALE consists of several devices installed across Italy, which collect data in the form of images or numbers, make a first processing and send them to a central server for storage, analysis and reporting. As shown in Figure 1, each peripheral device comes with two installation possibilities:
- ASTRALE Meteor: for those who have a good sky and visibility in all directions: the system is equipped with a Raspberry PI 4 camera for all-sky monitoring, as well as sensors for sky and air quality.
- ASTRALE Air: for those who lack a good sky, due to light pollution and / or reduced visibility, but wish to keep under control the quality of the air they breathe.
What makes ASTRALE unique?
- Automatic detection system: an auomtated detection tool has been developed to identify each transient event recorded by our devices. To date, over 10000 events have been visually inspected and classified by each volunteer citizen. This amount of data has been training an artificial intelligence algorithm that provides a real-time classification of each image. Citizen science is the driving engine to make this ambitious goal possible.
- Low-cost: As a non-profit association, we are fully committed to keep the cost as low as possible, while ensuring a high-quality performance. This cost simply matches the reimbursement for all hardware components purchased from the market. No earning is present, neither at personal nor at association level.
- User-friendly: our system can be distributed across Europe and easily installed at home, with no need for maintenance. The only requirements are Internet connection, a socket and an outdoor space. Our team provides full-time assistance to the user.
- Interdisciplinary: this project has blossomed from the close interaction between amateur astronomers, professionals, outreach providers, who are all part of AstronomiAmo. The ASTRALE project encompasses complementary fields of expertise, such as astronomy, environmental science, software engineering, science communication and citizen science. For this reason, ASTRALE aims at engaging the widest possible audience, driven by a common passion for science and environmental awareness.
How does it work?
Images are captured with a Raspberry HQ Cam with a 12.3 Mpixel Sony IMX477 and a CS-mount with a 2.5mm fisheye lens. A dew heater is used to keep the lens and the dome free of moisture. The camera is coupled with a Raspberry PI4 2GB single board computer with a Debian based Linux distribution. The control software is developed in Python and OpenCV. The camera also provides the Sky Quality Meter (SQM) to measure the brightness of the sky (in mag/arcsec2).
Temperature, pressure and humidity are measured by an I2C BME680, while a PMS5003 is used to measure particulate matter (PM1, PM2.5, PM10). The device is completed by the ozone MQ131 sensor and the MICS6814, a MEME sensor that can detect CO, NO2 and NH3. The air quality index (AQI) is then computed as the highest among the above concentration indices, where each can be measured on a daily or hour-moving average.
Our popular participation project Meteor Lens is inspired by the fantastic project of "Zooniverse", a worldwide platform for citizen science open to volunteers and enthusiasts. Figure 2 displays an all-sky snapshot taken from the webcam with a 20 sec integration exposure, reaching down to an apparent magnitude of 4.5. Our algorithm draws a rectangle around each transient object, sending an automatic alert with recording date, time and image coordinates.
Citizen science is crucial to help the ASTRALE system to better and better discriminate between celestial events related to meteors (Figure 2) and false positives related to clouds, reflections, lightning or passage of satellites and / or aircraft (see Figure 3). To this end, a self-explanatory tutorial guides the user on how to recognize different classes of events. “Lens'' refers instead to the flagship tool we provide for meteor recognition: a digital lens to increase the size of possible meteors (Figure 4).
What can you do for ASTRALE?
Meteorites are the oldest rocks in our Solar System and they represent a physical record of the formation and evolution of planet Earth. Observing the trajectory and colour of these bodies from multiple cameras allows us to calculate their velocity and path and, if a meteorite is recovered, give us key information around the origin of rocks and planets in the Solar System.
The improvement of the detection algorithm needs your participation! In order to achieve this goal, we have dedicated an area to anyone who wants to participate. The user will be given a list of images obtained from our cameras and will be asked to classify each of them.
If the sky conditions are not ideal for all-sky monitoring, the Astrale Air tool can be installed to measure the AQI (Figure 5). Those estimates provided by our device will expand the existing network supplied by the Regional Agency for Environmental Protection (ARPA) across the Italian territory, further tightening the monitoring of the air that we breathe.
How to cite: delvecchio, I., Capretti, S., Di Mario, L., Gulic, A., and Piccialli, A.: ASTRALE: an Artificial Intelligence and Citizen-Science driven project, Europlanet Science Congress 2024, Berlin, Germany, 8–13 Sep 2024, EPSC2024-1041, https://doi.org/10.5194/epsc2024-1041, 2024.
Abstract:
This study investigates the physical properties of asteroids using optical data obtained by the Unistellar network of citizen astronomers. Leveraging the extensive observations provided by hundreds of users, we aim to characterize the size, shape, and rotation properties of a diverse sample of asteroids. Our analysis encompasses data collected over multiple observing campaigns conducted between 2021 and 2024, focusing on both near-Earth and main belt asteroids. By combining photometric light curves and stellar occultations, we derive comprehensive physical models for these celestial bodies. Our findings contribute to a deeper understanding of the asteroid population and provide valuable insights into their formation and evolution.
Introduction:
Asteroids represent remnants of the early solar system and offer valuable insights into its formation and evolution. Studying their physical properties, such as size, shape, and rotation, is crucial for understanding their composition and origins. The Unistellar network of citizen astronomers comprised of over 10,000 telescopes provides a unique opportunity to collect large-scale optical data for a wide range of asteroids, enabling comprehensive studies of their physical characteristics.
Data and Methods:
We utilized optical data collected by the Unistellar network between 2021 and 2024, focusing on observations of both near-Earth and main belt asteroids. Photometric light curves and stellar occultations were used to derive the sizes, shapes, and rotation properties of the asteroids. We analyzed data from multiple observing campaigns that targeted specific asteroids of scientific interest. We utilized the convex inversion method developed by Mikko Kaasalainen.
Results:
Our analysis resulted in rotation state properties and detailed 3D models for tens of asteroids. We obtained accurate measurements of size, shape, and rotation period for numerous celestial bodies, shedding light on their individual characteristics and variability within the asteroid population. Additionally, we identified intriguing phenomena, such as concavities and asymmetric light curves, providing insights into the dynamical processes shaping these objects.
Conclusions:
The optical data obtained by the Unistellar network of citizen astronomers offers valuable insights into the physical properties of asteroids. By leveraging these observations, we have advanced our understanding of the asteroid population, contributing to ongoing efforts to explore the solar system's early history. Our study highlights the importance of citizen science initiatives in expanding our knowledge of celestial objects and their origins.
Figure 1. The Unistellar European network comprises citizen astronomers. As of May 2023, approximately 10,000 eVscopes are distributed globally, with over 3,000 of them located in Europe
Figure 2. The plot showcases light curve observations of asteroid (216) Kleopatra revealing variations in brightness over its rotation.
Figure 3. The plot showcases light curve observations of near-Earth asteroid (1627) Ivar revealing variations in brightness over its rotation.
How to cite: Hanus, J., Marchis, F., Lambert, R., Esposito, T., and Durech, J.: Exploring Asteroids: Unraveling Physical Properties Through Citizen Science Astronomy, Europlanet Science Congress 2024, Berlin, Germany, 8–13 Sep 2024, EPSC2024-591, https://doi.org/10.5194/epsc2024-591, 2024.
Summary
Long-term observations by amateur astronomers show that Jupiter’s major domains commonly show cyclic phenomena repeated for several decades, but which can then switch to a different mode of activity [ref.1]. Now these cycles can be characterised thoroughly by modern amateur imaging, complemented by spacecraft images which provide very-high-resolution images of the component features. This is exemplified by the South Temperate Belt (STB), which showed a consistent cyclic pattern of disturbances from 1998-2018, in which new structured sectors of STB would arise preceding oval BA and drift eastward and expand, eventually catching up with oval BA from the following side. From 2019-20 onwards, the style of the disturbances has changed although many consistent aspects remain. Here, we describe the origins of new cyclonic spots preceding Oval BA, similar to previous examples but observed closely by JunoCam. These provide well-studied models for the origins and metamorphoses of cyclonic spots not only in this domain but also in others. We also describe how the new spots have developed into structured segments, showing variations on the previous theme, and resulting in the revival of a dark STB around much of the circumference in a way not seen since the mid-1990s.
Introduction: The cyclic behaviour (1998-2018)
The merger of three large white ovals in 1998 and 2000 left only a single large anticyclonic oval, called BA. Major cyclonic features are ‘structured sectors’ of STB, separated by largely undisturbed sectors, and there are always between two and four of them. One is always a dark sector of STB following BA (STB Segment A), of variable length and activity. Each additional structured sector arose tens of degrees preceding BA, first seen as a small dark spot, then developed in one of two ways: either it would expand as a dark turbulent STB segment, or it would change from dark through reddish to white and then expand as a pale, quiescent loop. In either case, the new structured sector would drift eastward faster than BA and therefore eventually, after several years, having become tens of degrees long, it would collide with dark STB Segment A following BA. This collision caused vigorous activity (including, in two cases, a sudden convective outburst that transformed the formerly quiescent structured segment into a turbulent dark segment); and soon it would merge with Segment A, and emit streams of dark spots eastward (in the STBn jet) and westward. The reinvigorated Segment A would then shrink down towards BA again over one or more years.
All this is summarised in Figure 1 & Ref.2. There were five repeats of this cycle, creating structured segments designated sequentially from B to F.
Shift to a new regime
In 2019 there was just one structured sector apart from Segment A: a long pale loop called the ‘STB Spectre’ (Segment F). Unlike previous examples, it grew extremely long, so its following end was no longer approaching BA; and when its preceding end arrived at Segment A, in early 2020, it did not transform internally. Instead, Segment A itself grew more active and longer as it accelerated BA eastward, and initiated the usual streams of dark spots eastward and westward. The STB Spectre itself became unrecognisable.
Meanwhile, we were expecting one or more new cyclonic spot(s) to arise some way preceding BA to initiate the next structured sector. This eventually happened in 2020, with appearance of two dark spots which we named spots 6 and 7. Spot 7 would become the more important: a sudden convective outburst within it created “Clyde’s Spot”, a turbulent feature which has expanded continually from that time to become the new turbulent, dark STB Segment G [refs. 3&4]. As oval BA had accelerated to similar speed, the longitudinal cycle of successive segments has been broken. Instead, the expanding Segments A and G, and the streams of dark spots emitted from both of them, have led to re-creation of a visibly dark STB around much of the circumference (Figure 2).
Evolution of cyclonic spots
Spots 6 and 7, and a new Spot 8 which appeared in 2021, have all undergone various transformations during their lifetimes, intermittently observed close up by JunoCam. Even before 2020, JunoCam had revealed several small, pale cyclones in the whitened STB latitudes p. BA, and spots 6, 7, and 8 developed by transformation of these cyclones [ref.4]. Subsequently, they transformed variously between three canonical types of cyclonic circulation (e.g. Figure 3): dark oval (“mini-barge”); white oval (which may expand); and turbulent patch (“mini-FFR”, which may also expand, to become a dark STB segment). Figure 4 summarises the metamorphoses of these three spots.
The same three types of cyclonic circulation are common in other domains, with minor variations. In the S2 domain, where they are often longer oblongs, we have documented how each type can change into any other type [see our EPSC abstract in the OPS2 session].
Acknowledgements:
Some of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004).
Details of the observations are posted in regular reports on the JunoCam and BAA websites:
https://www.missionjuno.swri.edu/junocam; https://britastro.org/sections/jupiter
References:
1. J.H. Rogers, The Giant Planet Jupiter. CUP (1995).
2. J. Rogers et al., BAA reports on Jupiter’s South Temperate domain, 1991-1999-2012-2015-2018: https://britastro.org/node/17283 & refs. therein.
3. C. Foster et al., EPSC Abstracts (2020) no.196 & (2021) no.121.
4. R. Hueso et al., ‘Convective storms in closed cyclones in Jupiter’s South Temperate Belt: I. Observations.’ Icarus 380, 114994 (2022).
Figure 1:
Figure 2:
Figure 3:
Figure 4:
How to cite: Rogers, J., Hansen, C., Eichstädt, G., Orton, G., Momary, T., Adamoli, G., Bullen, R., Foster, C., Jacquesson, M., Vedovato, M., and Mettig, H.-J.: Jupiter’s South Temperate Domain: Origins of new cyclonic features and a change in the cyclic regime, 2019-2024, Europlanet Science Congress 2024, Berlin, Germany, 8–13 Sep 2024, EPSC2024-362, https://doi.org/10.5194/epsc2024-362, 2024.
We are presenting online tools for asteroids studies: the Ground-based Observational Service for Astroids (GaiaGOSA) (Santana-Ros et al., 2016) and Interactive Service for Asteroid Models (ISAM) (Marciniak et al., 2012). Both tools are used by both: amateur and proffesional astronomers. Nowadays, small telescopes are commonly used and they are located all over the world. This is a perfect situation for coordination of the observing campaigns and observations of space and time critical events. The service allows to upload raw observations taken by means of small telescopes.
The GaiaGOSA service is an online tool dedicated for amateur observers who want to support professional researchers in asteroid studies. The service is hosted in Astronomical Observatory Institute at Adam Mickiewicz University and all data are processed by researchers working there. There is always a list of objects visible from each location in the whole globe. Using developed tools observers can create an observing plan and establish the best strategy for observations. After taking observations the data are uploaded to the service and processed. Outcomes are presented in the GaiaGOSA (see Fig. 1), and the results are used for further studies of physical properties of asteroids. GaiaGOSA can be found at the website: gaiagosa.eu. GaiaGOSA provides a clear tutorial and a constant technical support for observers.
Fig1. An example of the lightcurve obtained by GaiaGOSA Observer.
On second presented tool ISAM, one can choose a polyhedral asteroid model and display its orientation for any requested date and in different modes (see Fig. 2), including stereoscopic views. One can also generate animations, both for the rotating model and the resulting lightcurve. Making predictions for the future light variations and object orientations is also possible. The latter is particularly useful in preparation of resolved observations such as stellar occultations or adaptive optics. ISAM can be found at http://isam.astro.amu.edu.pl/
Fig2. An example of the model of 89 Julia asteroid in the ISAM service.
Both services are a part of the Europlanet PARSEC Alert System (http://www.parsec-europlanet.eu), which was developped in the framework of Europlanet-2024-Ri project. The PARSEC (PlAnetaRy SciencE Collaboration tool) service is a tool for coordinating the Solar System observations for amateur observers and researchers. Parsec contains observational campaign coordination tool with alert system not only for asteroids but also for other Solar System Bodies.
References:
Santana-Ros, T. , Bartczak, P., Marciniak, a., 2016, The Minor Planet Bulletin (ISSN 1052-8091). Bulletin of the Minor Planets Section of the Association of Lunar and Planetary Observers, Vol. 43, No. 3, pp. 205-207
Marciniak A., Bartczak P. Santana-Ros T. et al. 2012, "Photometry and models of selected main belt asteroids IX. Introducing interactive service for asteroid models (ISAM)", Astronomy and Astrophysics, Volume 545, id.A131
How to cite: Podlewska-Gaca, E., Bartczak, P., Santana-Ros, T., Marciniak, A., Wilawer, E., and Langner, K.: Online services for asteroids studies , Europlanet Science Congress 2024, Berlin, Germany, 8–13 Sep 2024, EPSC2024-304, https://doi.org/10.5194/epsc2024-304, 2024.
The aim of the project is to create spin and shape models of selected main belt asteroids based on dense ground-based lightcurves and
the data from space missions.
Research on asteroids is important for understanding the origin and evolution of the whole Solar System. Studying them will allow us to
better understand the nature of asteroids. Knowledge of the physical properties of
asteroids will also facilitate future space mining. The basis for creating asteroid models are the photomrtric lightcurves, which allows for the
determination of various asteroid parameters. The data used to create these brightness changes come from observations conducted by both: professional
astronomers and amateurs. Such collaboration enables the accumulation of large amounts of data necessary for modeling.
Ground-based observations are also supplemented by data from space missions like TESS anf Gaia.
The main modeling tool is the SAGE program, developed in the Astronomical Observatory Institute at Adam Mickiewicz University.
Using genetic algorithm it enables to create non-convex spin and shape model for asteroids basing solely on lightcurves.
The first source of data is photometric observations of asteroids made by amateur astronomers, who submit the raw observations to the GaiaGOSA
service. Another source is data from the Roman Baranowski Telescope (RBT) located in Arizona, obtained by professional astronomers.
To create an accurate model, the data from multiple
opositions are necessary. Gathered observations display the view of asteroids from different phase angles and
ecliptic coordinates. Thanks to this we observe the amount of light incoming from different geometrical orientation of the object.
Using advanced genetic algorithm SAGE(Dudziński, & Bartczak, 2018) calculates
a good approximation of the three-dimensional shape of the asteroid, as well as its rotation period and the orientation of the rotation axis (pole position).
We have created the models for large main belt asteroids. Thanks to long and dense lightcurves from TESS mission we were able to determine
spin orientation and precise shapes of the asteroids. Moreover, the sparse data from Gaia mission allowed to determine the proper size of asteroids
along rotation axis. We are presenting here the results for 59 Elpis, 96 Aegle and 134 Sophrosyne. In Fig. 1 we show the calculated shape of 96 Aegle.
In the near future precise models for next objects will be determined.
Fig 1: Calculated shape model for 96 Aegle.
Bartczak, P. ; Dudziński, G. , "Shaping asteroid models using genetic evolution (SAGE)", 2018, Monthly Notices of the Royal Astronomical Society, Volume 473, Issue 4, p.5050-506
How to cite: Najda, K., Podlewska-Gaca, E., Bartczak, P., Takacs, N., Kiss, C., Bosh, J. M., Kamiński, K., Kamińska, M., and Polińska, M.: Determination of physical parameters of asteroids based on data from space and ground-based telescopes., Europlanet Science Congress 2024, Berlin, Germany, 8–13 Sep 2024, EPSC2024-340, https://doi.org/10.5194/epsc2024-340, 2024.