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październik/october 2024 |
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2024-10-04 |
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mgr SUBHRATA DEY |
Obserwatorium Astronomiczne UJ |
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Publiczna obrona pracy doktorskiej / Public PhD defense Panchromatic spectral energy distribution modeling of infared bright galaxies
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2024-10-11 |
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2024-10-18 |
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dr VASANTH VELUCHAMY |
Obserwatorium Astronomiczne UJ |
ZN OA 1606 |
Coronal Signatures of Flare Generated Fast-Mode Wave at EUV and Radio Wavelengths
We present a detailed case study of the type II solar radio burst occurred on 06 March 2014
using combined data analysis. It is a classical radio event consisting of type III radio burst
and a following type II radio burst in the dynamic spectrum. The type II radio burst is
observed between 235 – 130 MHz (120 – 60 MHz) in harmonic (fundamental) bands with
the life time of 5 minutes between 09:26 – 09:31 UT. The estimated speed of type II burst by
applying two-fold Saito model is ∼ 650 km/s. An extreme ultraviolet (EUV) wave is
observed with Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics
Observatory (SDO). The very close temporal onset association of the EUV wave and flare
energy release indicates that the EUV wave is likely produced by a flare pressure pulse. The
eruption is also accompanied by a weak coronal mass ejection (CME) observed with the
coronagraphs onboard the Solar and Heliospheric Observatory (SOHO) and the twin Solar
Terrestrial Relations Observatory (STEREO). The plane of sky speed of the CME was ∼ 252
km/s in the SOHO/LASCO-C2 and ∼ 280 km/s in the STEREO-B/SECCHI-COR1 images. The
EUV wave has two wave fronts, one expanding radially outward and the other one moving
along the flare loop arcade. The source position of the type II burst imaged by the Nançay
Radio Heliograph (NRH) shows that it was associated with the outward moving EUV wave.
The CME is independent of the shock wave as confirmed by the location of NRH radio
sources below the CME’s leading edge. Therefore the type II radio burst is probably ignited
by the flare. This study shows the possibility of EUV wave and coronal shock triggered by
flare pressure pulse, generating the observed type II radio burst.
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2024-10-25 |
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listopad/november 2024 |
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2024-11-01 |
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Wszystkich Świętych / All Saints Holiday
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2024-11-08 |
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godzina 11:30 / at 11:30 p.m. |
2024-11-15 |
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prof. JERZY KREINER |
UKEN, Kraków |
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O inicjatywach obserwacyjnych Tadeusza Banachiewicza
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godzina 12:00 / at 12:00 p.m. |
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prof. ALEKSANDER SCHWARZENBERG-CZERNY |
CAMK, Warszawa |
ZN OA 1607 |
Tadeusz Banachiewicz jako pionier informatyki w Astronomii i naukach pokrewnych
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2024-11-22 |
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mgr SEBASTIAN KUROWSKI |
Obserwatorium Astronomiczne UJ |
ZN OA 1608 |
150th anniversary of the Grubb refractor
The Grubb refractor, currently located in the southwestern dome of the
Cracow Observatory, is the oldest working instrument at the institute. It
was manufactured in 1874 in Thomas Grubb's factory in Dublin. However, the
history of this instrument at the Jagiellonian University begins much
later, in 1929, when Prof. Tadeusz Banachiewicz brought this telescope to
Cracow, where it became one of the main scientific instruments.
Now, celebrating the 150th anniversary of the Grubb refractor, we are
entering a new era of this instrument's service to the astronomical
community. Thanks to the new narrowband solar filters, it is becoming a
valuable teaching tool for astronomy students. In this talk I’ll present a
brief history of the Grubb refractor and show its current capabilities for
solar observations.
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2024-11-29 |
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dr PRATIK DABHADE |
Narodowe Centrum Badań Jądrowych, Warszawa |
ZN OA 1609 |
From unveiling Giant Radio Galaxies to harnessing them as astrophysical probes
Giant Radio Galaxies (GRGs) are home to active supermassive black holes that produce
powerful bipolar radio jets, creating structures that extend over megaparsec scales. These
are the largest structures in the Universe, growing up to Mpc-scales and even surpassing
the size of massive galaxy clusters. Though discovered 50 years ago, significant progress in
understanding GRGs has been made only in the past eight years, largely due to the advent
of sensitive sky surveys and the efforts of the SAGAN project ('Search & Analysis of GRGs
with Associated Nuclei').
Research continues to explore whether the immense size of GRGs is driven by their efficient
AGN or the sparser environments in which they reside. The SAGAN project, initiated in
2016, has produced several research papers, including a review, discovering the largest
samples of GRGs and refining our understanding of their key properties. The project has
rejuvenated global interest in these giant radio sources.
This seminar will review how our understanding of GRGs has evolved with deep radio
surveys like LoTSS, which have uncovered the largest and faintest GRGs. We will discuss
optical-infrared data from SDSS and WISE, revealing AGN accretion properties, and
millimetre-wave data from IRAM, offering insights into AGN fuelling. We will also showcase
GMRT radio images revealing previously unseen low-surface-brightness structures in GRGs,
enabling more precise age and magnetic field estimates. Lastly, we will demonstrate how
GRGs can be used as cosmic probes of large-scale environments and magnetic fields, with
key implications for understanding magnetogenesis.
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grudzień/december 2024 |
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godzina 14:00 / at 14:00 p.m. |
2024-12-06 |
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mgr AGNIESZKA MIROCHA |
Obserwatorium Astronomicze UJ |
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Publiczna obrona pracy doktorskiej / Public PhD defense Występowanie i własności promieniowania ultrafioletowego w obszarach powstawania gwiazd w Drodze Mlecznej
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2024-12-13 |
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dr SZYMON SIKORA |
Obserwatorium Astronomiczne UJ |
ZN OA 1610 |
Hubble tension
The growing precision and accuracy of the Lemaitre-Hubble constant determination recently lead to inconsistency between the
value of Lemaitre-Hubble constant derived by different methods. The CMB-based value is significantly lower than the value measured with
the help of the standard candles. In this presentation, I show the specific solution to the second-order cosmological perturbation
theory, which could partially explain the difference between the measured values of the Lemaitre-Hubble constant.
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2024-12-20 |
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2024-12-27 |
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przerwa świąteczna / Holiday break
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styczeń/january 2025 |
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2025-01-03 |
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przerwa świąteczna / Holiday break
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2025-01-10 |
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2025-01-17 |
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2025-01-24 |
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2025-01-31 |
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przerwa egzaminacyjna / Exam break
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luty/february 2025 |
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2025-02-07 |
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przerwa egzaminacyjna / Exam break
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2025-02-14 |
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ferie zimowe / Holiday break
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2025-02-21 |
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przerwa egzaminacyjna / Exam break
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2025-02-28 |
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mgr ADAM ZYCHOWICZ |
Obserwatorium Astronomiczne UJ |
ZN OA 1611 |
Bayesian Approach to Equipartition Estimation of Magnetic Field Strength
Magnetic fields, together with cosmic rays (CRs), play an important role in the dynamics and evolution of galaxies,
but are difficult to estimate. Energy equipartition between magnetic fields and CRs provides a convenient way
to approximate magnetic field strength from radio observations. In this talk I will present a new approach
for calculating the equipartition magnetic field strength based on Bayesian methods.
In this approach, the magnetic field is a random variable that is distributed according to a posterior distribution
conditional on synchrotron emission and the size of the emitting region. It allows for the direct application
of the general formulas for total and polarized synchrotron radiation without the need to invert these formulas,
which has limited the equipartition method to highly simplified cases. We have derived the equipartition condition
for the case of different low-energy breaks, slopes, and high-energy cutoffs of power-law spectra of the CR proton
and electron distributions. The derived formalism was applied in the general case of a magnetic field consisting of
both uniform and randomly oriented field components. The applied Bayesian approach naturally provides the uncertainties
in the estimated magnetic field strengths resulting from the uncertainties in the observables and the assumed values
of the unknown physical parameters. I will also present a web application BMAG that implements the described approach
for different models and observational parameters.
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marzec/march 2025 |
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2025-03-07 |
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prof. ANDRZEJ ZIĘBA |
Akademia Górniczo-Hutnicza, Kraków |
ZN OA 1612 |
Copernicus on atoms
Copernicus is associated with the study of objects on a cosmic scale. Only a few people know that
the manuscript of De revolutionibus contains a fragment of 56 latin words, in which we find the term “atoms”.
In it, Copernicus used the concept of the atom to formulate an additional argument for the extremely great
distance to the fixed stars.
I will try to answer different questions that arise. Why was this fragment not included in the Nuremberg
first edition of 1543 and the subsequent latin editions? How did Copernicus understand the concept of the atom?
How could he have known this hypothesis? How does his argument for the enormous distance to the stars look
in the light of contemporary knowledge?
Additionally, we will discuss Kepler's views on the discontinuous structure of matter, as presented in his 1611 work
Strena seti de nive sexangula (Eng: On Hexagonal Snowflakes), and the little-known fact of Rheticus's
stay in Kraków in the years 1554–1574.
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2025-03-14 |
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mgr KAMIL KASPRZAK |
Obserwatorium Astronomiczne UJ |
ZN OA 1613 |
RS Ophiuchi - The First VHE Gamma Ray Nova
Gamma-rays were not widely anticipated to be detected from novae.
Yet, the 2010 detection of V407 Cygni nova by Fermi-LAT Collaboration
was the evidence that gamma-ray emissions can occur from interactions
between nova shells and the medium inside the binary. Subsequently,
Fermi-LAT detected three different novae in High Energy Gamma-Rays (HEGR),
and the search for Very High Energy Gamma-Ray (VHEGR) emission started
-- with the first, and for now the only, VHEGR detection in August of 2021
from RS Ophiuchi recurrent nova, simultaneously and independently by MAGIC
and H.E.S.S. collaborations, as well as LST-1 of the Cherenkov Telescope
Array (CTA). In this talk, I will introduce the Cherenkov technique
for photon detection, shortly report on 2010-2013 HEGR nova detections,
describe current understanding of a nova outburst, and present my re-analysis
of the H.E.S.S. data of the 2021 RS Ophiuchi nova, as well as explain the event
reconstruction methods and compare my 2024 analysis to the original 2021 analysis.
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2025-03-21 |
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SESJA NAUKOWA Z OKAZJI 80. ROCZNICY URODZIN PROFESORA PIOTRA FLINA |
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Szczegóły wydarzenia
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2025-03-28 |
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kwiecień/april 2025 |
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2025-04-04 |
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2025-04-11 |
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dr hab. inż. PIOTR ORLEAŃSKI, prof. CBK/UJ |
Obserwatorium Astronomiczne UJ CBK PAN |
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Space mission safety, or anything bad that can happen when it shouldn't
Unfortunately, sometimes it happens, because:
1. space is a very hostile environment
2. in space, as a rule, we use things developed for the first time or
as a result of small-series production
3. no tests on Earth are able to fully simulate the real space environment
4. however, even if we could deal with all the problems mentioned above,
the main source of most disasters in space missions is still ourselves.
A person with his faith in his own perfection, a tendency to downplay details,
setting priorities that are not always adequate for a specific mission
or simply insufficient knowledge, generates the main part of the problems himself.
These issues will be the subject of a presentation by Piotr Orleański.
Several examples of major space missions (Chandrayaan-1, ROSETTA, BRITE, Herschel,
Beagle2/MarsExpress, Sciaparelli/ExoMars) in which the above-mentioned elements
were the cause of major in-orbit failures will be presented.
The causes of failures will be discussed, and the possibilities of removing some of them will be shown.
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2025-04-18 |
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Wielki Piątek / Holiday break
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2025-04-25 |
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maj/may 2025 |
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2025-05-02 |
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Dzień wolny na UJ / Holiday break
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2025-05-09 |
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REZERWACJA |
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2025-05-16 |
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REZERWACJA |
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2025-05-23 |
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2025-05-30 |
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czerwiec/june 2025 |
   
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2025-06-06 |
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2025-06-13 |
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2025-06-20 |
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piątek po Święcie Bożego Ciała / Holiday break
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2025-06-27 |
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przerwa egzaminacyjna / Exam break
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lipiec/july 2025 |
   
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2025-07-04 |
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prof. ANDRZEJ ZDZIARSKI |
CAMK PAN, Warszawa |
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Jets in accreting black-hole binaries
The most spectacular jets are observed from active galactic nuclei,
in particular from quasars. However, highly interesting jets are also
launched by accretion flows in stellar binaries containing a normal star
accreting onto a stellar-mass black hole. Such systems are analogs of quasars
on a much smaller scale, and are called microquasars. There are two distinctly
different types of jets in microquasars. Jets of the first type are steady,
and are launched during accretion states characterized by hard X-ray emission.
They are launched over weeks to months, but are observed only up to maximum
distances of about a 1/1000 of a parsec. Those of the other type are launched
on time scales of only a day during transitions of the accretion flow from
the hard to soft spectral states, but are observed as moving blobs up to a parsec scale,
i.e., up to ~1000 times larger distances. I will discuss possible causes
of this difference, the jet emission mechanisms, collimation, the presence
of electron-positron pairs, magnetic fields, bulk Lorentz factors and the jet power.
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sierpień/august 2025 |
   
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wrzesień/september 2025 |
 
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