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październik/october 2011 |
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2011-10-07 |
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prof. WOJCIECH DZIEMBOWSKI |
Obserwatorium Astronomiczne UW |
ZN OA 1320 |
Bohdan Paczyński, mój wybitny kolega |
2011-10-14 |
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2011-10-21 |
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2011-10-28 |
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mgr SZYMON SIKORA |
IF UJ |
ZN OA 1321 |
The total Galaxy mass estimated from the motion of the halo compact objects
The thin disk model, which is a nonstandard approach to the modeling of the spiral galaxy dynamics, will be presented in context of the motion of the halo compact objects located around the Milky Way. Because in the thin disk framework there is no dark matter nonbaryonic component, it is interesting does the motion of the halo compact objects is compatibile with the low Galaxy mass predicted by the disk model.
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listopad/november 2011 |
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2011-11-04 |
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dr JERZY KRZESIÑSKI |
Uniwersytet Pedagogiczny, Kraków |
ZN OA 1322 |
Funkcja jasności gorących białych karłów z przeglądu SDSS - nowe spojrzenie |
godzina 10:30 / at 10:30 a.m. |
2011-11-18 |
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dr LESZEK BLASZKIEWICZ |
Uniwersytet Warmińsko-Mazurski, Olsztyn |
ZN OA 1323 |
Masery kosmiczne |
2011-11-25 |
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prof. BOHDAN NOVOSYADLYJ |
Astronomical Observatory of the Ivan Franko University in Lviv |
ZN OA 1324 |
Scalar fields as dark energy: suitability and problems |
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grudzień/december 2011 |
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2011-12-02 |
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dr OLGA SERGIJENKO |
Astronomical Observatory of the Ivan Franko University in Lviv |
ZN OA 1325 |
Widmo mocy linii 21 cm w modelach kosmologicznych ze sterylnymi neutrinami jako ciemną materią |
2011-12-09 |
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prof. BOŻENA CZERNY |
CAMK Warszawa |
ZN OA 1326 |
Origin of the broad emission lines in active galaxies
Broad and strong emission lines are the basic signatures of active
galaxies. The lines allowed Maarten Schmidt in 1963 to reveil the
cosmological nature of quasars. However, the origin of the lines remained
unknown. In our recent paper (Bozena Czerny& Krzysztof Hryniewicz) we
showed that the underlying mechanism is the presence of the dust in the
accretion disk atmosphere. In particular, we demonstrated that for all
active galaxies, independently from their mass and accretion rate the
Broad Line Region starsts where the disk atmosphere, descreasing with the
distance from the black hole, crosses 1000 K. At such temperature the dust
can start to form, and the radiation pressure, acting very efficiently in
the presence of dust, pushes the massive outflow. High above the disk the
material becomes irradiated by the distant nucler emission, the dust
evaporates, and the matter not supported further by the radiation pressure
fall back onto the disk. Turbulence created in the process combined with
the rotational motion reproduce the observed emission line profiles.
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2011-12-16 |
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prof. PAWEŁ HAENSEL |
CAMK Warszawa |
ZN OA 1327 |
Pomiar masy PSR J1614-2230 i fizyka gęstej materii |
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styczeń/january 2012 |
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2012-01-13 |
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mgr MICHAŁ ECKSTEIN |
Instytut Matematyki UJ Kraków |
ZN OA 1328 |
Noncommutative Geometry and Cosmology
Noncommutative Geometry and Cosmology
Noncommutative geometry is a vast generalisation of the standard
differential geometry. Apart from its mathematical elegance it has numerous applications in physical theories. In my talk I
will present various different cosmological models based on noncommutative geometry. The talk will have a review character
and is addressed to non-experts.
Geometria nieprzemienna a kosmologia
Geometria nieprzemienna jest obszernym uogólnieniem standardowej geometrii różniczkowej. Oprócz matematycznej elegancji
teoria ta ma wiele zastosowań w modelach fizycznych. W moim referacie przedstawię różne modele kosmologiczne
bazujące na geometrii nieprzemiennej. Referat będzie miał charakter przeglądowy i jest adresowany do szerokiej
publiczności.
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2012-01-20 |
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prof. MICHAŁ HELLER |
Uniwersytet Papieski Jana Pawła II |
ZN OA 1329 |
Kosmologia Lemaitre'a |
2012-01-27 |
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mgr JOANNA KOZAKIEWICZ |
OA UJ |
ZN OA 1330 |
Schumann Resonance on Mars |
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luty/february 2012 |
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2012-02-03 |
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2012-02-10 |
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2012-02-17 |
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2012-02-24 |
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dr KENJI TOMA
prof. FUMIO TAKAHARA |
Osaka University, Japonia |
ZN OA 1331 |
Neutron Energy and Mass Injection Efficiencies for AGN Jets
AGN jets are considered to be produced by injecting magnetic and/or
thermal energies into the dilute polar region, where the mass loading
processes are essential for determining the jet properties. We discuss
the role of the relativistic neutrons escaped from the accretion flow
for the mass loading (as well as thermal energy injection).
If I have time, I would also talk on my recent work on the emission
process of Fermi-GRBs. |
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marzec/march 2012 |
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2012-03-02 |
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dr SEBASTIAN SZYBKA |
OA UJ |
ZN OA 1332 |
Gravitational interaction between two bodies
Recently, Chrusciel, Eckstein, Nguyen and I have shown that stationary I^+ regular two-component black holes do not exist in
axial symmetry. I will discuss the result and the history of the problem.
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2012-03-09 |
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2012-03-16 |
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2012-03-23 |
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prof. TSUTOMU T. TAKEUCHI |
Nagoya University, Japan |
ZN OA 1333 |
Dust Extinction Law of Star-Forming Galaxies through AKARI and GALEX
The relation between the ratio of infrared (IR) and ultraviolet (UV) flux
densities (the infrared excess: IRX) and the slope of the UV spectrum (β) of
galaxies plays a fundamental role in the evaluation of the dust attenuation of
star forming galaxies especially at high redshifts. Many authors, however, pointed
out that there is a significant dispersion and/or deviation from the originally
proposed IRX-β relation depending on sample selection. We reexamined the
IRX-β relation by measuring the far- and near-UV flux densities of the
original sample galaxies with GALEX and AKARI imaging data, and constructed a
revised formula. We found that the newly obtained IRX values were lower than the
original relation because of the significant underestimation of the UV flux
densities of the galaxies, caused by the small aperture of IUE. Further, since the
original relation was based on IRAS data which covered
a wavelength range of λ = 42-122 μm, using the data from AKARI which has
wider wavelength coverage toward longer wavelengths, we obtained an appropriate
IRX-β relation with total dust emission (TIR):
log ( LTIR / LFUV ) = log [ 100.4 ( 3.06 + 1.58 β ) - 1 ] + 0.22.
This new relation is
consistent with most of the preceding results for samples selected at optical and
UV, though there is a significant scatter around it. We also found that even the
quiescent class of IR galaxies follows this new relation, though luminous and
ultraluminous IR galaxies distribute completely differently as well known before.
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2012-03-30 |
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dr hab. MARIAN SOIDA |
OA UJ |
ZN OA 1334 |
Ruch samochodów w symulacjach numerycznych |
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kwiecień/april 2012 |
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godzina 11:00 / at 11:00 a.m. |
2012-04-13 |
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prof. ANDRZEJ KUS |
UMK Toruń |
ZN OA 1335 |
OCRA (One Centimeter Receiver Array) na 32m toruńskim radioteleskopie
Jednym z fundamentalnych zadań obserwacyjnej kosmologii, związanych
z analizą CMB, jest precyzyjne zbadanie wpływu emisji od wszystkich znanych
obiektów pomiędzy obserwatorem i CMB. Cała klasa tych obiektów zwanych
"foregrounds" obejmuje m.in. emisję rozciągłą i wpływ dyskretnych źródeł
Naszej Galaktyki oraz pozagalaktyczne galaktyki typu Starburst, AGN a także
efekty komptonizacji w materii gromad galaktycznych. Różne zidentyfikowane
przyczyny, które zmieniają lub mogą zmienić mierzony strumień, widmo
i polaryzację reliktowych fotonów, muszą być uwzględnione i precyzyjnie
usunięte.
Badanie ewolucji galaktyk dla dużych "z" samo w sobie jest ciekawym
wyzwaniem, więc badanie najdalszych, a więc także najsłabszych źródeł jest
ważnym celem. Własności fizyczne radioźródeł i ich kosmologiczna ewolucja,
w szczególności ich zmienność mają znaczący wpływ na dokładność pomiarów
anizotropii CMB.
W celu zbadania populacji słabych źródeł (w sensie odbieranego strumenia)
zbudowano i zainstalowano na 32m radioteleskopie CA UMK matrycę odbiorczą
OCRA.
W referacie przedstawiona będzie główna idea systemu OCRA oraz podsumowane
zostaną uzyskane dotychczas wyniki badań. Dotyczą one źródeł galaktycznych
i AGN-ów a także efektu S-Z na 30 GHz (długość fali 1cm), wszystko
w kontekście wyznaczenia właściwości i wpływu "foregrounds".
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2012-04-20 |
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prof. JEAN-PIERRE LASOTA-HIRSZOWICZ |
OA UJ |
ZN OA 1336 |
Black holes spin |
2012-04-27 |
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mgr IWONA KOTKO |
OA UJ |
ZN OA 1337 |
AM CVn stars - a source of information about accretion disk physics |
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maj/may 2012 |
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2012-05-11 |
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dr MAREK KUBICKI |
Instytut Geofizyki PAN |
ZN OA 1338 |
Relacje Słońce - Ziemia na podstawie badań Globalnego Obwodu Elektrycznego |
2012-05-18 |
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mgr MAŁGORZATA SIUDEK |
Centrum Fizyki Teoretycznej PAN |
ZN OA 1339 |
Infrared composition of the Large Magellanic Cloud |
godzina 11:00 / at 11:00 a.m. |
2012-05-25 |
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dr hab. AGNIESZKA POLLO |
OA UJ |
ZN OA 1340 |
Highlights from VIPERS: on the way to precise measurements in the z~1 Universe |
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czerwiec/june 2012 |
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2012-06-01 |
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dr SABRINA CASANOVA |
Max Planck Institute, Heidelberg, Niemcy |
ZN OA 1341 |
Gamma-ray emission from molecular clouds |
godzina 11:00 / at 11:00 a.m. |
2012-06-15 |
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mgr inż. ANNA BARNACKA |
CAMK Warszawa |
ZN OA 1342 |
The gravitational lensing effect in gamma-rays |
2012-06-22 |
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mgr MICHAŁ PIRÓG |
Instytut Fizyki UJ |
ZN OA 1343 |
Co wiemy o dysku akrecyjnym w NGC 4258 |
2012-06-29 |
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lipiec/july 2012 |
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sierpień/august 2012 |
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wrzesień/september 2012 |
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2012-09-04 |
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Prof. DOMINIK BOMANS |
AIRUB, Bochum, Niemcy |
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Supernovae without Host Galaxies - from Low Surface Brightness Galaxies to Hypervelocity Stars
Galaxies with low stellar surface brightness (LSB galaxies) constitute
a important parallel branch of galaxy evolution (in addition to the
"normal" high surface brightness galaxies). Results from optical
searches for LSB galaxies imply that the number density distribution
stays flat out to a central surface brightness of 26
Bmag/sq-arcsec. Beyond that value, little known up to now. Even within
these limits, the currently known LSB population is already a
significant contributor to the local baryon density. In my talk I will
discuss a new search technique, using supernovae (SNe) as signposts for
extreme LSB galaxies. I will present results from our searches and discuss
implications for core collapse SNe and the existence of an extremely
dim LSB galaxy population. One unexpected result of our study is
the detection of SNe without any detectable host galaxy, but
relatively close to massive spiral galaxies. An attractive
explanation for these SN could be explosions from massive hyper
velocity stars, which would manifest the first occurrence of the
phenomenon beyond the Local Group of galaxies. This lead to
implications for the probability of hypervelocity stars and the
ionization of gas in the halos of galaxies.
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2012-09-14 |
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mgr TOMASZ KUNDERA |
OA UJ |
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ASTROGRID-PL |
seminarium nadzwyczajne: czwartek godzina 10:00 / at Thursday 10:00 a.m. |
2012-09-27 |
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prof. JÓZEF I. SMAK |
CAMK |
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Superwybuchy nowych karłowatych |
2012-09-28 |
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prof. ANDRZEJ ZDZIARSKI |
CAMK |
ZN OA 1344 |
Cyg X-1 i Cyg X-3: nowe wyniki |