Seminaria Instytutowe 2018/2019
Seminaria odbywają się co tydzień, w czwartki o godz. 13:00 w budynku Obserwatorium Astronomicznego UAM przy ul. Słonecznej 36. Osobą odpowiedzialną za ustalanie terminów i tematów wystąpień oraz za przebieg seminariów jest dr hab. Tomasz Kwiatkowski.
Informacje dla prelegentów.
Wystąpienia w poprzednich latach: 2017/2018, 2016/2017
18 kwietnia 2019
Seminarium odwołane
25 kwietnia 2019
mgr Volodymyr Troiansky (IOA)
Basaltic V-type asteroids and their fragments are collisional remnants of planetesimals that existed 4 billion years ago. Their distribution, physical and dynamical properties provide important constrains on processes such as planetary differentiation, planet formation and evolution of planetary systems.
Asteroids with the prograde sense of rotation, located in the inner Main Belt, that have semi-major axes of their orbits smaller than that of Vesta, are less likely to have migrated from Vesta due to thermal forces dragging them outwards (the Yarkovsky effect).
Assuming that the inner Main Belt is populated only by the Vesta like objects, around 81% of asteroids in the so-called scattered resonances region are expected to have retrograde sense of rotation. Similarly 40% of objects in the low inclination region, should have retrograde rotation. Substantial surplus of asteroids that have prograde rotation could indicate that also other planetesimals (different from Vesta) contributed to this population. Those predictions are verifiable via photometric studies in which asteroid lightcurves are used to derive senses of rotation.
9 maja 2019
prof. Tomasz Kwiatkowski (IOA)
NPDT: a web based service for determination of asteroid rotation periods from their lightcurves
16 maja 2019
mgr Jacek Haponiak (IOA)
23 maja 2019
30 maja 2019
mgr Piotr Guzik (OA UJ)
6 czerwca 2019
mgr Emil Wilawer (IOA)
13 czerwca 2019
W roku akademickim 2018/2019 wystąpili:
4 kwietnia 2019
prof. Piotr Dybczyński (IOA)
Na temat pierwszego makroskopowego gościa z przestrzeni międzygwiazdowej ukazało się dotąd prawie 60 publikacji. Obserwowało go kilkanaście najpotężniejszych teleskopów naziemnych i orbitalnych. Niestety tak krótka wizyta skutkuje wielkimi lukami w wiedzy na temat tego obiektu a to co wiemy przynosi nam więcej zagadek niż odpowiedzi. Posunięto się nawet w poważnej literaturze astronomicznej do sugerowania sztucznej natury tego obiektu jako tworu obcej cywilizacji. Większość badaczy jednak odrzuca takie spekulacje. Obiekt ten świetnie pasuje do swej nazwy — jest równie dziwny i tajemniczy.
28 marca 2019
mgr Patrycja Bagińska (IOA)
Rozbłyski nowych rentgenowskich (Soft X-ray Transients; X-ray Novae) są powodowane przez niestabilność jonizacyjną zachodzącą w zewnętrznych rejonach dysku akrecyjnego. Rozbłyski pojawiające się w wyniku tej niestabilności przyjmują charakterystyczny kształt związany z szybkim wzrostem jasności i jej eksponencjalnym zanikiem (profil FRED – fast rise exponential decay). Moja praca obejmowała badanie układów rentgenowskich, których obiektami centralnymi są czarne dziury. W ramach moich badań policzyłam modele rozbłysków przy pomocy kodu uwzględniającego ewolucję niestabilności w dysku akrecyjnym, strukturę wertykalną dysku oraz parametr lepkości. Utworzona przeze mnie baza modeli obejmowała różne kombinacje parametrów takich jak masa czarnej dziury, tempo akrecji czy krok czasowy i została utworzona dla ustalonego składu chemicznego dysku akrecyjnego (skład typu słonecznego). Dodatkowo wykonałam symulacje krzywych stabilności i modeli dla różnych składów chemicznych dysków akrecyjnych, żeby ustalić, z jakiego typu dyskami mamy do czynienia w obserwowanych obiektach. Zmiana składu chemicznego dysku (zwiększenie zawartości metali) powoduje powstawanie chaotycznych rozbłysków o niesymetrycznej strukturze, które pasują do danych obserwacyjnych. W wyniku dopasowania modeli do obserwacji uzyskałam potwierdzenie, że mechanizmem odpowiedzialnym za powstawanie rozbłysków w badanych systemach jest niestabilność jonizacyjna. W wyniku modelowania możliwe było również oszacowanie masy obiektu centralnego (czarnej dziury) i tempa akrecji na zewnętrznej części dysku.
21 marca 2019
mgr Mikołaj Krużyński (IOA)
Budowanie katalogu satelitarnego związane jest z systematycznymi obserwacjami ponad 20 tysięcy obiektów. Wymagana jest duża precyzja obserwacji pozycji satelity oraz precyzyjny pomiar czasu. Trzeba również uwzględnić szereg sił perturbujących, które mają wpływ na orbitę satelity. Do uwzględnienia tych wszystkich efektów niezbędne jest odpowiedni proces przeprowadzenia obserwacji i ich redukcji oraz specjalistyczne oprogramowanie. Chociaż obserwacje obiektów satelitarnych są wykonywane od ponad 60 lat, to wykorzystanie teleskopów w przypadku obiektów poruszających się poniżej 2000 km nad powierzchnią Ziemi jest nowością. Dopiero rozwój technologiczny, który nastąpił przez ostatnią dekadę, pozwolił na wykonywanie odpowiedniej jakości obserwacji astrometrycznych satelitów na orbitach typu LEO (Low Earth Orbit). I chociaż wciąż najdokładniejsze pomiary satelitarne wykonuje się przy użyciu dalmierzy laserowych to zakres ich użycia oraz wysoki koszt stanowią pewne ograniczenie w ich stosowaniu. Dlatego wykorzystanie pomiarów laserowych i astrometrycznych dla satelitów na orbitach LEO może prowadzić do uzyskania jeszcze lepszych wyników pomiarowych, a co za tym idzie jeszcze lepszego wyznaczenia orbity obserwowanego satelity. W czasie wystąpienia zostaną zaprezentowane wstępne wyniki pokazujące możliwość łączenia danych obserwacyjnych wykonanych przy użyciu różnych technik pomiarowych.
14 marca 2019
dr hab. Michał Michałowski (IOA)
I will present the results of observations (including those with RBT/PST2) of a gamma-ray burst (GRB) 171205A and the associated supernova (SN) 2017iuk, which led to the discovery of a hot gas cocoon. This was possible because observations started very early and the jet emission was weak. This gives support to the theoretical models of GRB/SN explosions, which predicted the existence of such a cocoon. This discovery opens the possibility to study internal processes during explosions of very massive stars, and hence will shed light on the understanding of the production of heavy elements. In case you miss this seminar, I will also give it at the Faculty of Physics on 3rd of April:
http://zon8.physd.amu.edu.pl/~miran/seminars.html
24 stycznia 2019
prof. Mirosław Giersz (CAMK PAN)
I will very briefly describe the basic ideas behind the Monte Carlo MOCCA code and discuss the set-up of the MOCCA Survey Database project – a database containing thousands of Monte Carlo (MOCCA) simulations of real globular clusters. Afterwards, I will list and shortly describe projects connected with the analysis of the Database from the point of view of compact objects. Projects which deal, among others, with: BH and NS populations in star clusters and their interactions, BH Subsystems and IMBHs and their observational signatures, and many more. Finally, I will discuss recent developments of the MOCCA code and planed simulations for the MOCCA Survey Database II.
17 stycznia 2019
mgr Krystian Iłkiewicz (CAMK PAN)
Cataclysmic variables (CVs) are interacting binary stars that consists of a degenerate white dwarf accreting mass from a normal star donor. Our understanding of evolution of such systems have been challenged by properties of their known population, such as white dwarf mass distribution, orbital period distribution and their space density. With the recent developments of population synthesis codes we are able to reproduce the CV population characteristics. However, there are still unsolved problems posed by the population of classical novae among the CVs, such as for example why there is only one system known to have both dwarf nova and classical nova outbursts. In my talk I will discuss the recent developments of population synthesis codes as well as my work on understanding of classical novae population using population synthesis.
10 stycznia 2019 (dwa krótsze referaty)
mgr Aleksandra Leśniewska (IOA)
Binary stars are very important topic of astrophysical research. Using the data from photometric and spectroscopic observations, we are able to determine much more physical parameters of the system’s components than in the study of a single star. We obtain information not only about effective temperatures, metallicity, rotation velocity, but what is the most important, masses and radii of two components. Compact binaries become crucial when considering the evolution of stars and their influence on the later generations of astronomical objects. The system composed of a white dwarf and a red giant, is called symbiotic star. Researches on these types of objects contribute to a more accurate understanding of the geometry of binary stars and mechanisms in these systems. Our work is dedicated to modeling the physical parameters of the SY Muscae, symbiotic star in the southern sky. Based on photometric and spectroscopic observational data, in the infrared and visible range, using the PHOEBE program we created a model of light curves and radial velocity. This model clearly describes the shape and dimensions of the components of SY Muscae. The result of the analysis is a model of light curves, radial velocity, and a set of SY Muscae physical parameters. Based on the comparison of the results obtained by us with the results in the literature, it turns out that SY Muscae is a typical symbiotic star.
Dust production is a very important issue in galaxy evolution. Unfortunately, we are still unable to determine its formation mechanism. I will present the investigation of dust production in nine galaxies at the redshift at z > 6, for which dust emission has been detected. In recent years, more accurate measurements were made using the most powerful instruments, eg ALMA, which contributed to better estimates of luminosities and sizes, and thus to determine the masses of gas, dust and stars in the studied galaxies. We conclude that asymptotic giant branch (AGB) stars did not contribute to the dust formation significantly in these Early Universe galaxies, and that supernovae are unlikely to produce the bulk of the dust mass. I will discuss how the advent of future large telescopes will contribute to this topic.
21 grudnia 2018 (Dodatkowe seminarium o 13:30 dla chętnych)
dr Anna Kapińska (National Radio Astronomy Observatory, USA)
The new continuum radio surveys delivered in recent years are an outstanding resource in addressing long-standing questions in modern astrophysics. In this talk I will focus on the lowest radio frequencies (<230MHz) currently accessible with the ground based new-generation radio facilities. Specifically, I will present our recent results on radio spectral energy distributions and star formation of Sculptor Group galaxies and Magellanic Clouds, which we observed with the Murchison Widefield Array (MWA) — a low frequency SKA precursor from an Australian outback. Although of low angular resolution, especially as compared to ALMA, these sensitive low frequency observations are very complementary to GHz observations, and necessary for a complete picture of physical processes occurring in galaxies.
20 grudnia 2018
dr Agata Makieła (University of Kent, UK)
In the summer 2017 I was involved in the NASA Frontier Development Lab, an intense 8-week study concentrated on tackling topics important to NASA using machine learning tools. During the programme interdisciplinary teams of early career researchers were looking at issues related to planetary defence, space weather, and space resources. The team I was a part of investigated shape modelling of near-Earth asteroidsfrom radar data. These asteroids are the Earth’s closest neighbours in space, most accessible by space flight and with a potential for causing a threat to the planet. Even though they are constantly monitored, detailed characteristics, like shapes and sizes, are available for only a selected few. Physical models are required to successfully plan spacecraft missions and set up impact mitigation strategies. Additional incentive is in learning know how our space environment works and evolves. Reconstructing asteroid shapes and spins from radar data is, like many inverse problems, a computationally intensive task. Shape modelling also requires extensive human oversight to ensure that computational methods find physically feasible results. In this talk I will discuss the results of our work at NASA Frontier Development Lab 2017, exploring the application of machine learning tools to the shape modelling task.
13 grudnia 2018
dr Krzysztof Hełminiak (CAMK PAN)
In years 2015-2017 we have conducted a programme of high-resolution spectroscopic observations of a sample of detached eclipsing binaries (DEBs) observed by the Kepler satellite in its original mission field. With the 1.88-m telescope of the Okayama Astrophysical Observatory and its HIDES spectrograph, we have collected 290 spectra of 23 systems, in order to analyse them thoroughly and as comprehensively as possible. The sample contains variety of different objects (giants, low-mass stars, multiples, pulsators, planet hosts), many of which were studied for the first time, and with parameters derived very precisely. In my semi-formal talk I will present a subjective selection of 10 systems from our sample that I find the most interesting, intriguing and important for the stellar astrophysics. Kittens will be included.
10 grudnia 2018 (Dodatkowe seminarium o 16:00 dla chętnych)
dr José Ricardo Rizzo Caminos (Centro de Astrobiologia, Madrid)
Opportunities using radio astronomy facilities in Madrid
6 grudnia 2018
dr Arkadiusz Hypki (IOA)
GAVIP-GridComputing (shortly GAVIP-GC) is an ESA project run by Poznan Astronomical Observatory staff which will add additional features to the Gaia archive by incorporating CPU power of volunteers’ computers of the BOINC grid (best known of its SETI@Home project). GAVIP-GC eventually will allow to define a series of jobs which will be able to read entire Gaia archive and compute some CPU intensive jobs on the BOINC platform. The users, in order to use the GAVIP-GC software will have to provide only source code to deal with their scientific problem. Everything else (e.g. reading data from Gaia, communicating with BOINC) will be done by GAVIP-GC software. During the seminar I will present the current status of the project and our plans for the next milestones.
29 listopada 2018
prof. David Vokrouhlický (Astronomical Institute of Charles University, Prague)
Asteroid families are clusters of small bodies that move about the Sun on fairly similar orbits. They are outcome of a collisional disruption of a common parent asteroid. Therefore, analysis of members in families can bring us interesting information about the fragmentation process at high-energies and, otherwise inaccessible, interior properties of asteroids. The most valuable in this type of studies are young families, in which the evolutionary processes had not enough time to confuse the results. I will review the past two decades of a race to find ever younger families in the main belt, demonstrating also what kind of unexpected results it brought along.
22 listopada 2018
prof. Edwin Wnuk (IOA)
Od 2019 roku Polska jako kraj członkowski Europejskiego Konsorcjum EU SSA (Space Situational Awareness) rozpocznie świadczenie usług SST (Space Surveillance and Tracking). W związku z tym, od pewnego czasu trwają intensywne prace, których celem jest zbudowanie Polskiego Systemu PL SST, który w przyszłości zostanie rozszerzony do PL SSA.
SSA składa się z trzech następujących segmentów:
Space Weather (SWE) – monitorowanie Słońca, wiatru słonecznego oraz ziemskiej magnetosfery, jonosfery i termosfery,
Near-Earth Objects (NEO) – detekcja i monitorowanie ruchu orbitalnego obiektów naturalnych, takich jak planetoidy i komety, które mogą zbliżać lub zderzyć się z Ziemią,
Space Surveillance and Tracking (SST) – detekcja, śledzenie i monitorowanie ruchu orbitalnego aktywnych i nieaktywnych satelitów oraz śmieci kosmicznych.
Polski System SST będzie składał się z Narodowego Centrum Operacyjnego (NOC), sieci kilkunastu teleskopów optycznych oraz stacji laserowej w Borowcu. Będzie ściśle powiązany z systemami EU SST i ESA SST oraz z europejskim centrum danych satelitarnych SATCEN. System PL SST, w pierwszym okresie działania, będzie świadczył dwie usługi dla EU SST: RE – Re-Entry oraz FR – Fragmentation, a później także CA – Collision Avoidance. Na potrzeby tych serwisów, a także na potrzeby krajowych odbiorców usług SST, będą wykonywane obserwacje wybranych obiektów satelitarnych, wyznaczane orbity tych obiektów oraz będzie tworzony i aktualizowany Katalog Satelitarny.
W referacie zostaną przedstawione aktualne informacje związane z tworzeniem systemu PL SST, w szczególności struktura organizacyjna i potrzeby softwarowe Centrum Operacyjnego. Opisane zostaną także krótko podstawowe serwisy SST, a także problemy związane z tworzeniem Katalogu Satelitarnego.
15 listopada 2018
prof. Jerzy Krzesiński (OA UJ)
We are showing that some of the exoplanetary signatures found in the light curves of a couple of sdBV star systems (KIC 5807616 and KIC 10001893) might be of different source than exoplanet light reflection or radiation effects. We point out that at least one signature can be explained by a combination of pulsating frequencies of the host star and others might be just artifacts. Using simulated light curves we also analyzed frequency changes of the signal around 0.256 c/d (~3.9 day) visible in the Fourier transform of the KIC 10449976 sdO star light curve. Our simulations show that it is difficult to reproduce the observed signal frequency variations by the weather changes in the exoplanet atmosphere.
8 listopada 2018
dr Justyna Gołębiewska (IOA)
From the launch of the first artificial satellite: Sputnik in 1957, more than 5000 launches have placed 8000 satellites into orbit, of which about 4800 remain in space. In addition to operational satellites in orbit there are over 12000 space debris. To to ensure safety in space European Space Agency (ESA) as well as European Commission carries out the Space Situational Awareness (SSA) Programme, consisting of three segments. One of these segments is the Space Surveillance and Tracking (SST) system that comprises detecting,cataloguing and predicting the orbits of objects orbiting the Earth, and related applications. We are showing our results in two of main segment of SST: Re-entry Predictions for Risk Objects and Collision Warning.
25 października 2018
prof. Tadeusz Jopek (IOA)
Wyszukiwano grupy pomiędzy planetkami typu NEA. Zastosowano dwie D-funkcje oraz rygorystyczny algorytm analizy skupień. Zidentyfikowano kilka nowych grup – obiektów poruszających się po orbitach z niewielkimi wartościami MOID względem orbity Ziemi.
18 października 2018
dr Krzysztof Kamiński (IOA)
In recent years European Space Agency (ESA) as well as newly established European Space Surveillance and Tracking Consortium (EU SST) — both of witch Poland is a member state — have increased the effort towards a new satellite tracking system for Europe, that would be independent from external sources of satellite orbital data. Such a system is typically composed of several radar sensors for tracking Low Earth Orbit (LEO) satellites and several optical sensors for higher orbit targets. However recent developments in optical telescopes enabled an efficient tracking of LEO satellites with an equipment 2 to 3 orders of magnitude cheaper than a typical satellite radar. Of course optical satellite sensing suffers from a daytime and bad weather limitations to a much greater extent than a satellite radar. Therefore it is reasonable to simulate an optical satellite tracking network, using a global cloud-fraction statistics, in order to estimate possible outcome from such an entertainment. In this seminar I present preliminary results of simulations showing weather it is possible to build an efficient global optical satellite tracking network, what locations should be selected on Earth, and how many sites should be used in order to have a very high probability of observing each target every day.
11 października 2018
dr hab. Agnieszka Pollo (OA UJ)
I will present recent results from the VIMOS Public Extragalactic Redshift Survey (VIPERS). VIPERS – with its \sim 90,000 spectroscopically measured galaxies, a large volume (5 x 10^7 h^(-3) Mpc^3), and an effective spectroscopic sampling > 40% – can be considered the state-of-the-art counterpart of „local” (z<0.2) cosmological surveys but targetting the epoch at z \sim 1. I will summarize our newest results on the properties of galaxies and large scale structure and their common evolution since z \sim 1. How galaxies changed during the last 8 bln years? What are the properties of the 3D cosmic structure emerging from VIPERS measurements and what they can they tell us about cosmological parameters? And, most interestingly – what remains unknown and why do we need even larger surveys in the future?
4 października 2018
Sprawy organizacyjne
W roku akademickim 2017/2018 wystąpili:
21 czerwca 2018
mgr Grzegorz Dudziński (IOA)
The volume of an asteroid shape model, when combined with the size and mass estimates, is essential in bulk density determination – one of the most important physical parameters that allow us to peek inside asteroids and make conclusions about their inner structure. The shape model uncertainty propagates to volume, and analogously to any
other property determined from the model, affecting every conclusion drawn for a population of small bodies under scrutiny. There definitely exists a compelling need for a procedure of quality and uncertainty assessment of asteroid models. I would like to present modelling-technique-independent uncertainty assessment method based on gen-
erating clones of investigated model. By far, the most abun-dant data type for the most numerous target sample is disc-integrated relative photometry in visual bands and the majority of published asteroid models are based solely on it. For that reason the presented method deals with photometric lightcurves and absolute sparse data.
14 czerwca 2018
dr Milena Ratajczak (IA UWr)
Several aspects of stellar evolution can be tested with B-type stars in eclipsing binary systems. Finding tighter constraints on the value of the convective core overshooting parameter is one of the most valuable among them. Precise photometry and high-resolution spectroscopy with high SNR are required to achieve that goal, but since many of the targets are bright enough, the challenge is fair. The approach to examine the aforementioned aspect of stellar evolution using observations of B-type stars obtained with a wide range of spectrographs, as well as BRITE-Constellation satellites, will be presented.
7 czerwca 2018
dr Magdalena Otulakowska-Hypka (IOA)
The disk instability model attributes the outbursts of dwarf novae to a thermal-viscous instability of their accretion disk, an instability to which nova-like stars are not subject. We aim to test the fundamental prediction of the disk instability model: the separation of cataclysmic variables (CVs) into nova-likes and dwarf novae depending on orbital period and mass transfer rate from the companion. We analyse the lightcurves from a sample of ~130 CVs with a parallax distance in the Gaia DR2 catalogue to derive their average mass transfer rate. The method for converting optical magnitude to mass accretion rate is validated against theoretical lightcurves of dwarf novae. Dwarf novae (resp. nova-likes) are consistently placed in the unstable (resp. stable) region of the orbital period – mass transfer rate plane predicted by the disk instability model. None of the analyzed systems present a challenge to the model. These results are robust against the possible sources of error and bias that we investigated. The disk instability model remains the solid base on which to construct the understanding of accretion processes in cataclysmic variables.
24 maja 2018
mgr Przemysław Mróz (OA UW)
Theories of planet formation predict the existence of a population of unbound (free-floating) planets. Gravitational microlensing provides a unique tool for studying these objects. The first results of Sumi et al. (2011) claimed that Jupiter-mass free-floating planets are as common as main-sequence stars. However, these results appear to disagree with censuses of substellar objects in young clusters and star-forming regions and with predictions of planet formation theories. I will present new results of the analysis of a ten times larger sample of microlensing events discovered by the OGLE-IV survey during the years 2010-2015. They shed new light on the population of free-floating planets.
17 maja 2018
mgr Ewa Kosturkiewicz (IOA)
Wstępne wyniki spektroskopowej kampanii obserwacyjnej gwiazdy delta Ceti w latach 2014 – 2017
10 maja 2018
mgr Krzysztof Langner (IOA)
Transformacja Kustaanheimo-Stiefela (KS) pozwala zregularyzować zagadnienie dwóch ciał i sprowadzić je do liniowej postaci oscylatora harmonicznego. Regularyzacja polega na zmianie zmiennej niezależne (czasu) i pozwala między innymi zwiększyć dokładność obliczeń numerycznych, zwłaszcza w przypadku orbit o dużym mimośrodzie. Transformacja Lissajous pozwala wprowadzić zmienne kąt działanie dla oscylatora harmonicznego. W trakcie prezentacji przedstawione zostanie połączenie obu transformacji, używając formalizmu kanonicznego oraz ich rozszerzenie pozwalające stosować ten formalizm w przypadku orbit z zaburzeniem jawnie zależnym od czasu.
26 kwietnia 2018
dr Agnieszka Słowikowska (CA UMK)
In my talk, I will describe the basic concept of polarimetry as well as the most common use of it as a tool in astronomy. I will present a few polarimeters that are in use at the moment. Additionally, I will discuss our recent polarimetry study of white dwarfs and neutron stars.
19 kwietnia 2018
prof. Andrzej Niedzielski (CA UMK)
Stars beyond the MS are frequently avoided in planet searches because they are known to exhibit various types of variability: RV variations of unknown origin were pointed out to be common in red giants (RGs) by Walker et al. (1989), and multiple pulsation modes are often present. In addition, the rotation of starspots across the stellar disk can affect the spectral line profiles of these stars (Vogt et al. 1987; Walker et al. 1992; Saar & Donahue 1997). However, soon after the first discovery (ι Dra b Frink et al. 2002), searches for planets around stars beyond the MS have become recognised as important in building a complete picture of planet formation and evolution for several reasons. First, they allow extending the reach of the most versatile RV technique, which is not applicable on the MS because of the high effective temperature of the stars and their fast rotation rates, to objects with masses significantly higher than solar (e.g., o UMa, a 3 M⊙ giant with a planet – Sato et al. 2012). Second, the planetary systems around evolved stars are much older than those around MS stars, and therefore they are suitable for long-term dynamical stability considerations. Planetary systems around giants are also subject to changes induced by stellar evolution, and therefore are suitable for studies of star – planet interactions, and last but not least, evolved planetary systems carry information on the initial population of planetary systems to be found around white dwarfs. It is no surprise then that several projects devoted to searches for RV planets that orbit RGs were launched. One of the largest of them is the PennState – Toruń Centre for Astronomy Planet Search (PTPS, Niedzielski et al. 2007; Niedzielski & Wolszczan 2008a,b).
In my talk I will present the sample of PTPS, current status of our planet search and the most recent discoveries. I will also discuss some properties of the exoplanets around evolved stars from the PTPS perspective.
12 kwietnia 2018
prof. Agata Różańska (CAMK)
X-ray astronomy requires satellites to make progress in searching the distribution of hot matter in the Universe. Approximately 15 years period of time is needed for full construction of the flight instrument from the mission concept up to the launch. A new generation X-ray telescope ATHENA (the Advanced Telescope for High Energy Astrophysics) was approved by European Space Agency as a large mission with a launch foreseen in 2028. I will talk about how ATHENA will help us to study Hot and Energetic Universe, and I will present Polish involvement to the mission development.
5 kwietnia 2018
dr Michał Drahus (OA UJ)
Disruptions of asteroids are often viewed as ancient events leading to the
formation of asteroid families and pairs, binary and multiple systems, and
discrete dust bands within the Zodiacal cloud. But thanks to the
remarkable progress in solar system science over the last decade, we can
now directly observe asteroidal disruptions occurring before our eyes.
Various lines of evidence suggest that the disruption can be a consequence
of a rapid rotation resulting from a long-term spin-up, or a result of a
hypervelocity collision with another minor object. Up until recently the
two mechanisms were difficult to distinguish because of the unknown
rotation rates of the disrupting small asteroids, but this has changed
after our team investigated the recently disrupted asteroid P/2012 F5.
Using the Keck II telescope atop Mauna Kea we discovered several fragments
of the object and obtained the highly anticipated measurement of the
rotation rate, which turns out to be the fastest known among active
asteroids and is fast enough to support the rotational disruption
scenario. Further observations with the Hubble Space Telescope have
revealed that the system is in fact the first ultra-young asteroid family
identified to date, and given its likely formation via rotational
disruption, it can also be the first known asteroid family of
non-collisional origin.
22 marca 2018
prof. Agnieszka Kryszczyńska (IOA)
The NEO-DECS web service an open access central service of structured
metadata on NEOs, as well as a platform for collaboration among NEO
researchers, using elements well known in social networking like user
profiles, forum facility, private messaging, etc. Such service shall make
it easy to locate necessary databases and services on NEOs, learn about
forthcoming conferences and workshops, and allow for advertising new
observing programs, telescopes availability, numerical tools, etc.
During the talk I will demonstrate NEO-DECS based on several use cases.
15 marca 2018
Seminarium odwołane
8 marca 2018
prof. Edwin Wnuk (IOA)
Polska Agencja Kosmiczna przygotowała projekt Krajowego Programu Kosmicznego
(KPK) i przedstawiła jego pierwszą wersję w grudniu 2017 r. Po
konsultacjach z różnymi zaineresowanymi środowiskami KPK ma być zatwierdzony
do realizacji w pierwszym kwartale 2018 r., po czym maja być ogłoszone
pierwsze konkursy merytoryczne obejmujące szeroki zakres zagadnień z zakresu
badań kosmicznych, w tym również z zakresu astronomii.
W trakcie wystąpienia seminaryjnego zostaną przedstawione podstawowe
informacje o KPK, zostaną omówione trzy projekty priorytetowe KPK oraz
wymienione zostaną obszary zagadnień, w których zostaną rozpisane konkursy
grantowe. Podane zostaną też podstawowe informacje dotyczące zasad
wnioskowania o projekty KPK oraz informacje o planowanym budżecie KPK.
Przedstawione na seminarium informacje będą dotyczyły głownie obszarów
naukowego i edukacyjnego w KPK.
1 marca 2018
dr Magdalena Polińska (IOA)
We would like to present results for the two objects, GT UMa B which is a part of multiple system and for the eclipsing binary star BD-00 2862. The spectra for the first object were obtained with the spectrograph ESPERO mounted on the 2-m telescope in Rozhen and for the second one with PST1 (Poznań Spectroscopic Telescope 1) located in Borowiec. For those stars we estimated atmospheric parameters, such as: the effective temperature, surface gravity, metallicity and the projected rotational velocity. The observed spectra were compared with the set of synthetic spectra calculated with the iSpec code.
22 lutego 2018
dr Arkadiusz Hypki (IOA)
The amount of data in science which is delivered nowadays increases like never before. It applies for all fields of research. However, physics and astrophysics appear to push the requirements for data storage and analysis to the boundaries. With already existing missions like Gaia and for future projects like LSST the need for reliable and scalable data storage and management is even higher. The amount of data for many projects is too big for simply processing with bash or python scripts. Tools which would allow easy data analysis are crucial in research these days.
BEANS software is a web based, easy to install and maintain, new tool for interactively distributed data analysis. It provides a clear interface for querying, filtering, aggregating, and plotting data from an arbitrary number of datasets and tables.
During the seminar I will present features of the BEANS software and show how it can help scientists to analyze huge datasets.
25 stycznia 2018
dr An-Li Tsai (IOA)
Galactic molecular outflows affect star formation activities in galaxies. This process is important for galaxies evolution. I will talk about case studies on two nearby starburst galaxies NGC 2146 and NGC 3628.
18 stycznia 2018
prof. Joanna Mikołajewska (CAMK)
I will present and discuss recovery of the binary underlying the classical nova of 11 March 1437 recorded by Korean royal astronomers whose age is independently confirmed by proper motion-dating. I will also discuss the physical characteristics and the present evolutionary status of the binary system responsible for the nova outburst based on preliminary results of our ongoing extensive observations.
11 stycznia 2018
prof. Michał Ostrowski (OA UJ)
New gamma-ray observatories: Cherenkov Telescope Array (CTA)
4 stycznia 2018
dr Dagmara Oszkiewicz (IOA)
SANORDA (Service for Archival NEO Orbital and Rotational Data Analysis) is an ESA funded project aimed at archiving light curve and orbital data. In work package WP1200 we focus on determining historical orbits of all NEOs to reproduce their orbital improvement history starting from discovery onwards. The historical orbits may aid better observation planing and improve our understanding of astrometric biases present in the Minor Planet Centre database. We focus on two orbit computation methods: the ranging method and the traditional linearised least squares method. For asteroids with short observational arcs (shortly after discovery) we use ranging method and when the phase space of possible orbital solutions is sufficiently contained (close to Gaussian distribution) we switch to least squares. Those orbital histories are being reproduced for around 17 000 NEAs, which will result in almost 2 000 000 orbits. The project is ongoing and the final database is expected in 2018.
14 grudnia 2017
prof. Sławomir Breiter (IOA)
Poczwórny układ gwiazdowy w rezonansie 1:1
7 grudnia 2017
prof. Piotr Dybczyński (IOA)
O pochodzeniu międzygwiazdowego obiektu A/2017 U1
30 listopada 2017
dr hab. Tomasz Kwiatkowski (IOA)
A new catalogue of asteroid lightcurves
23 listopada 2017
dr Przemysław Bartczak (IOA)
Niepewności modeli planetoid
16 listopada 2017
prof. David Vokrouhlický (Astronomical Institute of Charles University, Prague)
Origin and evolution of short-period comets
9 listopada 2017
dr Krzysztof Kamiński (IOA)
Nowa poznańska kamera satelitarna
26 października 2017
dr Michał Michałowski (IOA)
Pierwsze obserwacje promieniowania wysyłanego przez zderzające się gwiazdy neutronowe – źródło fal grawitacyjnych
19 października 2017
dr Paweł Kankiewicz (IF UJK, Kielce)
Dynamika planetoid na orbitach wstecznych
12 października 2017
dr Anna Marciniak (IOA)
Pierścień wokół planety karłowatej Haumea oraz jej rozmiary, kształt i gęstość z obserwacji zakrycia gwiazdowego
Wystąpienia w roku akademickim 2016/2017:
8 czerwca 2017
mgr Mikołaj Krużyński (IOA)
Obserwacje sztucznych satelitów nie tylko przy użyciu PST2
1 czerwca 2017
dr Toni Santana-Ros (IOA)
Ménage à quatre projektów europejskich związanych z badaniem planetoid
25 maja 2017
mgr Krzysztof Langner (IOA)
Nowe podejście do transformacji Kustaanheimo-Stiefela
18 maja 2017
mgr Ewa Kosturkiewicz (IOA)
Badanie gwiazd pulsujących typu beta Cephei
11 maja 2017
dr Michał Michałowski (IOA)
Pył, galaktyki i błyski gamma
27 kwietnia 2017
mgr Patrycja Bagińska (IOA)
Nowe rentgenowskie: analiza i modelowanie rozbłysków
20 kwietnia 2017
mgr Magda Butkiewicz-Bąk (IOA)
Fotometria planetoid w gęstych polach gwiazdowych
6 kwietnia 2017
dr Anna Marciniak (IOA)
Fotometria, modelowanie i skalowanie planetoid o długich okresach i niskich amplitudach
30 marca 2017
prof. Tadeusz Jopek (IOA)
Spadek łańcuszkowy meteorytu Morasko
23 marca 2017
dr Magdalena Polińska (IOA)
Badania spektroskopowe gwiazd delta Scuti
16 marca 2017
prof. Witold Szczuciński (IG UAM)
Geologiczne i środowiskowe skutki małego uderzenia meteoroidu – wnioski z badań w rejonie Moraska
9 marca 2017
mgr Łukasz Gruszka (IOA)
Wyniki projektu LTDS związanego z dystrybucją czasu lokalnego
2 marca 2017
dr Krzysztof Kamiński (IOA)
Pakiet programów do planowania i redukcji obserwacji astrometrycznych Sztucznych Satelitów Ziemi
23 lutego 2017
dr Przemysław Bartczak, mgr Grzegorz Dudziński (IOA)
GAVIP-GC
dr Wojciech Dimitrow (IOA)
Relacja z „Warsztatów praktycznych ESO”
26 stycznia 2017
mgr Grzegorz Dudziński (IOA)
Status prac nad SAGE; inwersja obserwacji radarowych planetoid
12 stycznia 2017
dr Jerzy Nawrocki (OAG CBK PAN, Borowiec)
Uruchomienie fontanny cezowej w Borowcu
15 grudnia 2016
dr hab. Tomasz Kwiatkowski (IOA)
The olivine-dominated composition of the Eureka family of Mars Trojan asteroids
8 grudnia 2016
dr Krzysztof Kamiński (IOA)
Obserwacje SST za pomocą PST1 i PST2
24 listopada 2016
prof. David Vokrouhlický (Astronomical Institute of Charles University, Prague)
Tilting Saturn during planetary migration
17 listopada 2016
dr Jan Janik (Masaryk University, Brno)
Gorące gwiazdy w Brnie
10 listopada 2016
mgr Filip Berski (IOA)
Bliskie przejście gwiazdy Gliese 710
3 listopada 2016
dr Przemysław Bartczak (IOA)
Wyznaczanie kształtu planetoidy z krzywych zmian blasku i danych radarowych metodą SAGE
27 października 2016
dr Arkadiusz Hypki (Leiden Observatory)
MOCCA – current state and [Breiter] future ahead
20 października 2016
dr Dagmara Oszkiewicz (IOA)
Searching for parent bodies of anomalous HEDs
13 października 2016
dr Magdalena Otulakowska-Hypka (IOA)
Ciasne układy podwójne
6 października 2016
Michał Żołnowski, Grzegorz Duszanowicz, Marcin Gędek,
Michał Kusiak, Rafał Reszelewski (6ROADS)
Obserwacje SST i NEO przy pomocy sieci teleskopów 6ROADS
