AstronomicalAstronomical Institute in the High TatrasInstitute in the High Tatras
Study, science and career pathStudy, science and career path
Martin Vaňko
Astronomical Institute, Slovak Academy of Sciences
Tatranská Lomnica 059 60, Vysoké Tatry
• Lomnický štít, 2 632 m. • Stará Lesná, 815 m. • Skalnaté Pleso, 1 786m.
The History of InstituteThe History of Institute
 Climatologist and Astronomer
* Stará Boleslav 1901 - † Brandýs n. Labem 1965
 Building an observatory at Skalnaté Pleso
(1941-1943).
 First observation at Skalnaté Pleso – solar
photosphere – solar spots on September 19th, 1943
The History of InstituteThe History of Institute
 Atlas Coeli Skalnaté Pleso (1951)
published by Sky Publishing
Corporation as the Skalnate Pleso
Atlas of the Heavens Skalnaté
Pleso (1951)
 The next Atlases:
Atlas Eclipticalis, 1950.0 (1958)
Atlas Borealis, 1950.0 (1962)
Atlas Australis, 1950.0 (1964)
 Position of 32 571 stars and other objects (clusters, galaxies...)
The History of InstituteThe History of Institute
The History of InstituteThe History of Institute
The History of InstituteThe History of Institute
 The highest place in Slovakia where people live and work (2632m a.s.l.)
 Building an observatory at Lomnický štít (1957-1962)
 20/300 cm ZEISS coronograph: The first observation of solar prominences in 1962 and the first
observation of solar corona in 1964.
The History of InstituteThe History of Institute
 1979-1985: The main building of Astronomical Institute, Slovak Academy of Sciences
 People: 32 scientific fellows, 2 PhD. students, 57 people in total
 Science: The Sun, Variable stars, Exoplanets, Interstellar matter
The History of InstituteThe History of Institute
Departments and InfrastructureDepartments and Infrastructure
Stellar DepartmentStellar Department
Department of Interstellar MatterDepartment of Interstellar Matter
Department of Solar PhysicsDepartment of Solar Physics
Stellar DepartmentStellar Department
SD includes 12 scientific fellows and 3 technicians/observers
SD: fields of study:
A) Interacting binaries/Symbiotic starsA) Interacting binaries/Symbiotic stars
Physical processes during different stages of symbiotic stars activity:
mass accretion and outflow, bipolar jets, ionization and radiation
scattering in the nebula.
B) Binaries and Multiple Stellar systemsB) Binaries and Multiple Stellar systems
Close binary stars in general, Contact binaries, Active (spotted) binaries, short period group
of RS CVn-like systems, Multiple systems of stars with an eclipsing component, Post-commonenvelope
binaries (with a SD or WD component), High-speed photometry-occultations
C) ExoplanetsC) Exoplanets
Observations: -radial velocities, -planetary transits, -timing
convection, day-night heat transfer, chemistry of low temperatures, secondary eclipses, Brown
dwarfs
Department of Interstellar MatterDepartment of Interstellar Matter
Here we have 11 researchers, 2 PhD. students and 2 technicians/observers
Asteroids, Comets and MeteoroidsAsteroids, Comets and Meteoroids
- P- Photometry of asteroids: leads to the search for double asteroids and the determination of their
physical parameters (composition, sizes, shapes, rotation).
- Photometry of comets: activity of selected cometary nuclei at larger distances from the Sun
its influence on the physical and dynamic evolution of these bodies is also carried out in order to
understand the production of dust, the morphology of tails, etc.
- Investigation of near-Earth meteoroid populations, including the mass distribution of particles in
meteoroid streams and their background, the internal structure of the streams, their age and
evolution.
- The Earth's environment is mapped and the composition of meteoric particles entering the Earth's
atmosphere is studied using observations from 4 stations of the European Bolide Network in
Slovakia, including the spectral bolide camera in Stará Lesna.
- The origin and formation of the Oort cloud, # The dynamical evolution of the small bodies of the
Solar system
Department of Solar PhysicsDepartment of Solar Physics
DSP has 10 people and 3 technicians/observers
Magnetism, the dynamics and variability of the solar atmosphereMagnetism, the dynamics and variability of the solar atmosphere
# the study of the solar photosphere and chromosphere and active phenomena
# using modern spectro-polarimetric, spectroscopic and photometric observations obtained with
solar telescopes of the highest world level (Gregor, VTT, SST, THEMIS) and satellites as well
# the study of the solar corona and its structures (prominences, coronal holes, condensations) and
# the study of Sun-Earth relations using data obtained with modern infrastructure at Lomnický štít
observatory
# the study of processes and propagation of energy during active phenomena in the solar
atmosphere, mutual connections between large-scale manifestations of solar activity (eruptions,
coronal mass ejections, EUV waves).
Instrumentation – Stará Lesná observatoryInstrumentation – Stará Lesná observatory
Telescope:Telescope: 61cm (24 inch) Zeiss Jena Cassegrain reflector (f = 750cm)
DetectorDetector: CCD kamera FLI ML 3041, filtre UBVRI (Bessell), chip
2048×2048, pixel size 15×15 μm, FoV 14′×14′.
Instrumentation – Stará Lesná observatoryInstrumentation – Stará Lesná observatory
BD And
J221550.6+495611 in NGC 7243 - candidate
XO-6b
Instrumentation – Stará Lesná observatoryInstrumentation – Stará Lesná observatory
Telescope:Telescope: 61cm (24 inch) Zeiss Jena
Cassegrain reflector (f = 750cm)
eShel spectrographeShel spectrograph design & parameters
-Littrow design with f/5, prism cross-disperser, 125mm collimator
-fiber-fed, R2 échelle grating, 79 grooves/mm, spectral resolution R=11000
-useful spectral range: 24 orders covering 4100-7600 Å, 50 micron object
fiber, 200 micron calibration fiber,
-calibration lamps: ThAr, Tungsten, blue LED
-CCD detector: ATIK 460EX camera, f/6 FIGU, WATEC 120n guiding cam.
Instrumentation – Stará Lesná observatoryInstrumentation – Stará Lesná observatory
1
2
3
1 – calibration unit
2 – FIGU Fiber Injection and
Guide Unit
3 – spectrograph
Instrumentation – Stará Lesná observatoryInstrumentation – Stará Lesná observatory
Instrumentation – Stará Lesná observatoryInstrumentation – Stará Lesná observatory
Instrumentation – Skalnaté Pleso observatoryInstrumentation – Skalnaté Pleso observatory
Vacuum facility for coating mirrors (aluminium, silver,
protective layers)
Instrumentation – Skalnaté Pleso observatoryInstrumentation – Skalnaté Pleso observatory
Telescope:Telescope: 1.3m Nasmyth-Cassegrain reflector (f=10.4m); ASTELCO Systems GmbH, Germany
Detector:Detector: MUSICOS = Multi-SIte COntinuous Spectroscopy, fiber-fed and optical bench-mounted
- Littrow design, FIGU, fibers & calibration lamps from Shelyak, 31.6 lines/mm, R2 échelle, 128x254mm
- 56 orders covering 4190-7200 Å (limited by the chip size), spectral resolution R=38000,
- magnitude limit V=11, SNR=15 in 15 minutes exposure.
Brightness-limited RV precision is about 20 m/s for MUSICOS while only 160 m/s for
eShel for a 9 mag star
beta Per, between H-beta & H-alpha
Instrumentation – Skalnaté Pleso observatoryInstrumentation – Skalnaté Pleso observatory
Instrumentation – Skalnaté Pleso observatoryInstrumentation – Skalnaté Pleso observatory
Observing projects at both spectrpgraphs:Observing projects at both spectrpgraphs:
-symbiotic stars and novae
-close binaries, multiple systems of stars
-T Tauri objects
-CP stars (mostly cooper. with Ernst Paunzen)
-exoplanet host stars
-follow-up observations for BRITE satellite object
RV variability of τ Boo
data between March
13 and June 6, 2014
rms = 78 m/s
K = 461.1 m/s
P = 3.312 days
RV variability of HAT-P-2b
data between March 14 and
July 3, 2014
5 points between phases
0.2 and 0.4
rms = 326 m/s
K = 983.9 m/s
P = 5.633 days
Easy to record emission lines but risk of saturation in Hα, spectrophotometry
Instrumentation – Skalnaté Pleso observatoryInstrumentation – Skalnaté Pleso observatory
Telescope:Telescope: 0.61-m f/4.3 Newtonian reflector
Detector:Detector: CCD SBIG ST-10XME + Johnson-Cousins UBVRI
-size of CCD pixels&chip 6.8 microns square, 2184 x 1472
pixels
-dark Current 0.5e-/pixel/sec at 0 °C
-A/D Gain 1.3e-/ADU
-read Noise 8.8e¯ RMS
-field of view 19.5’ x 13.1’, resolution 0.535”/px (1x1 binning),
1.069”/px (2x2 binning)
Photometry of comets and asteroidsPhotometry of comets and asteroids
Instrumentation – Skalnaté Pleso observatoryInstrumentation – Skalnaté Pleso observatory
Low amplitude of PHA asteroid 1981 Midas
Instrumentation – Skalnaté Pleso observatoryInstrumentation – Skalnaté Pleso observatory
Comet C/2020 F3 NEOWISE and its
structures close to the nucleus
Faint interstellar
comet 2I/Borisov
0.61-m, R filter, 2019 09 13 1.3-m, R filter, 2019 10 18
1.3-m, R filter, 2019 10 20 0.61-m, R filter, 2019 12 09
Instrumentation – Lomnický štít observatoryInstrumentation – Lomnický štít observatory
Telescope(s):Telescope(s): two coronographs: ZEISS 200/3000 : D=20 cm, f=4 m
Detectors:Detectors: Coronal Multi-channell Polarimeter (CoMP-S)
Solar Chromospheric Detector (SCD)
Instrumentation – Lomnický štít observatoryInstrumentation – Lomnický štít observatory
An example of a quiescent prominence, observed on October 20, 2012 near the south pole
of the Sun sequentially in the spectral lines of H I 656 nm and Ca II 854 nm
(top - H I 656 07:08:40 UT, bottom Ca II 854 nm 07:04:43 UT).
Instrumentation – Lomnický štít observatoryInstrumentation – Lomnický štít observatory
Evolution of an eruptive prominence, observed on March 10, 2014 above the southeast limb
of the Sun (AR 11991) in the spectral lines H I 656 nm (06:58:22, 07:24:12, 08:04:49 UT left
to right.
Instrumentation – Lomnický štít observatoryInstrumentation – Lomnický štít observatory
Example of an eruptive prominence, observed on March 10, 2014 above the southeast limb
of the Sun (AR 11991) in the 10 minute time interval sequentially in 4 spectral lines:
Na I 587 nm (08:25:17 UT), H I 656 nm (08:21:53 UT), Ca II 854 nm (08:19:35 UT),
and He I 1083 nm (08:15:59 UT) - top to bottom.
Instrumentation – Lomnický štít observatoryInstrumentation – Lomnický štít observatory
Evolution of an eruptive prominence, observed on July 13, 2014 above the southeast limb
of the Sun (near AR 12107) high above the solar limb together with an apparent
'solar tornado' close to the solar limb in the spectral line H I 656 nm
(05:09:42, 05:18:30, 05:27:02 UT - left to right).
CooperationCooperation
 D. Dunlap Observatory, Canada
 Ondřejov Observatory – Czech Republik
 Masaryk Uni. Brno – Czech Republik
 University Graz - Austria
 Astrophysical Institute Jena, Germany
 European Northern Observatory, Canaries,
Spain
 Astrophysical Institute, Potsdam, Germany
 Observatory Tautenburg, Germany
 ...and others
PhD. studyPhD. study
-Registration for each semester of PhD study is at Comenius University, Faculty of
Mathematics, Physics and Informatics in Bratislava.
-Astronomical Institute is in this case a training workplace
-Duration of the PhD study is four years
-Stipendium ~ 950-1000 EUR/month
-The possiblity to work in the field of observing and also theoretical astrophysics.
-Institute can provide also accommodation in Vila Tatra – Tatranská Lomnica)
Academic year 2023/2024: PhD. topicsAcademic year 2023/2024: PhD. topics
Stellar Physics and ExoplanetsStellar Physics and Exoplanets
1. Doubly and multiply eclipsing systems
Supervisor: Dr. Theodor Pribulla (pribulla@ta3.sk)
Objectives: Detection and modeling doubly and multiply eclipsing systems. Determination of the
orbital and absolute parameters of the components. Including fine light-curve effects in the
modeling of eclipses.
2. Exoplanets transiting early-type stars
Supervisor: Dr. Theodor Pribulla (pribulla@ta3.sk)
Objectives: Detection of transiting exoplanets showing transit duration changes (TDV). Realistic
modeling of exoplanet transits in rapidly rotating stars including fine light-curve effects (exact
stellar and planetary shapes, Doppler beaming, gravity darkening). Finding the wavelength effects
on the transit light curves relevant for the upcoming mission ARIEL.
Academic year 2023/2024: PhD. topicsAcademic year 2023/2024: PhD. topics
Stellar Physics and ExoplanetsStellar Physics and Exoplanets
3. Formation of young stars of T Tauri type and their planetary systems
Supervisor: Dr. Martin Vaňko (vanko@ta3.sk)
Objectives: Follow-up observations for candidate T Tauri stars and modelling of binary components
containing a few Myr young stars to determine their physical parameters, rotational periods, character
and nature of the observed photometric variability. Acquiring of multicolour photometry (including much
desired U-band) of selected T Tauri stars.
Solar physicsSolar physics
4. Solar activity cycles – empirical implications for the solar dynamo modelling
Supervisor: Dr. Ján Rybák (choc@ta3.sk)
Objectives: An expected output of the research is determination of the temporal evolution of the timelatitude
asymmetry of the solar activity for time period of several solar activity cycles and an analysis of
its importance for different periods together with searching for probable periodicities of the activity.
Academic year 2023/2024: PhD. topicsAcademic year 2023/2024: PhD. topics
Interstellar matterInterstellar matter
5. Distribution of the orbits of sporadic meteoroids
Supervisor: Dr. Mária Hajduková (Maria.Hajdukova@savba.sk@ta3.sk)
Objectives: The aim of this work is to map the sporadic background, based on models and the synthesis
of observations obtained by different techniques. Observations from Earth of the sporadic background
(and its representation in a coordinate system centered at the Earth’s apex) have revealed six apparent
sources in which enhanced meteor densities are observed: the so-called helion and antihelion sources,
the northern and southern apex sources, and the northern and southern toroidal sources. The distribution
of radiants is geometrically determined, but different types of comets or asteroids can be found
associated with different regions of enhanced density.
Academic year 2023/2024: PhD. topicsAcademic year 2023/2024: PhD. topics
Interstellar matterInterstellar matter
6. Modelling of asteroid activity in terms of rotation, 3D shape and tail morphology changes
Supervisor: Dr. Marek Husárik (mhusarik@astro.sk)
Objectives: Analysis of the activity of a normally inactive body with respect to the orientation of the
rotation axis in space, with respect to its shape, possible precession or surface albedo variegation.
Computational modelling of tail formation and morphology based also on own observations.
7. The origin and formation of the inner Oort cloud
Supervisor: Dr. Marián Jakubík (mjakubik@astro.sk)
Objectives: The main aim of this work is detailed description of the origin and formation of inner Oort
cloud with main emphasis on models describing the formation of the Oort cloud in its birth star cluster.
In more detail, we will solve open questions of this process using numerical simulations with respect of
recent observations. Among answers on various open questions, we will find the solution of particular
problem related to high number of objects (in the inner Oort cloud) revolving around Sun on retrograde
orbits resulting from previous numerical simulations.
Academic year 2023/2024: PhD. studyAcademic year 2023/2024: PhD. study
https://www.astro.sk/en/study/phd-study/https://www.astro.sk/en/study/phd-study/
Thank you !Thank you !
Acknowledgement: This work was supported by the Slovak Research and Development Agency under contract No. APVV-20-0148