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1

Evolution of Polish hydrogeology

Kozerski B., Paczyński B., Sadurski A., Skrzypczyk L.

Przegląd Geologiczny

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2010

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Vol. 58, nr 9/1

730-736

EN

In Poland, hydrogeology as a separate scientific discipline came into being at the end of the 19th century. The first geologists were interested in springs, saline, mineralised waters of therapeutic use and dewatering of mines. Until World War I, in the early stages of hydrogeological developments, a different attitude towards groundwater problems was clearly notable in all three annexed Polish territories. The next stage of the development of Polish hydrogeology is dated to the years 1918-1939. In those times, the major focus of hydrogeological investigations was on building structures to extract artesian groundwater; mineral groundwater in the Polish spas; building municipal water intakes; and on Quaternary aquifers, widespread in Poland. Early hydrogeological handbooks were published at those times. The contemporary stage of Polish hydrogeology started in 1945, after World War II. In the early 1950s, the Department of Hydrogeology and Engineering Geology was established at the Central Board of Geology (CUG in Polish), which belonged to the Polish government as a separate ministry up to 1970. Hydrogeological companies with technology and development sections were founded in big cities. Nowadays, academic centres exist in Warsaw, Cracow, Wrocław, Gdańsk, Sosnowiec, Poznań, Kielce and Toruń. About 1400 persons with academic diplomas, 160 doctors and 22 professors of hydrogeology are active at present in the field of hydrogeology. The principal fields of Polish hydrogeology comprise the following: mine dewatering, recognition of groundwater resources and their protection, construction and exploitation of water intakes, hydrogeological cartography, mineral and thermal water resources, regional hydrogeology for physical planning, groundwater modelling and groundwater pollution, migration of pollutants and forecasting of groundwater changes. Up to the late eighties, political censorship was the main difficulty for the development of Polish hydrogeology, especially in publications related to sensitive information of groundwater occurrence and resources.

2

Coronal Activity from the ASAS Eclipsing Binaries

Szczygieł D. M., Socrates A., Paczyński B., Pojmański G., Pilecki B.

Acta Astronomica

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2008

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Vol. 58, No. 4

405--418

EN

We combine the catalog of eclipsing binaries from the All Sky Automated Survey (ASAS) with the ROSAT All Sky Survey (RASS). The combination results in 836 eclipsing binaries that display coronal activity and is the largest sample of active binary stars assembled to date. By using the (V-I) colors of the ASAS eclipsing binary catalog, we are able to determine the distances and thus bolometric luminosities for the majority of eclipsing binaries that display significant stellar activity. A typical value for the ratio of soft X-ray to bolometric luminosity is L_X/L_bol≈ a few ×10^-4, similar to the ratio of soft X-ray to bolometric flux F_X/F in the most active regions of the Sun. Unlike rapidly rotating isolated late-type dwarfs - stars with significant outer convection zones - a tight correlation between Rossby number and activity of eclipsing binaries is absent. We find evidence for the saturation effect and marginal evidence for the so-called ``super-saturation'' phenomena. Our work shows that wide-field stellar variability searches can produce a high yield of binary stars with strong coronal activity.

3

The Distance to Pleiades

Paczyński B.

Acta Astronomica

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2003

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Vol. 56, No. 2

209--211

EN

The distance to Pleiades remains controversial. There is a simple way to resolve the dispute definitely by measuring the distance to one of its brightest members, Atlas, which is an astrometric and spectroscopic binary.

4

Systemy nieprzeobrażonych antropogenicznie zwykłych wód podziemnych Polski

Paczyński B.

Biuletyn Państwowego Instytutu Geologicznego

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2002

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nr 400

37-55

PL

Głębsze systemy zwykłych wód podziemnych, dobrze izolowane, o naturalnym składzie chemicznym i właściwościach fizycznych, stanowiące swoiste pomniki przyrody, wymagają szczególnej ochrony i racjonalnego użytkowania.

EN

Fresh groundwater of apparently natural chemical composition and physical properties, which occurs in aquifer-systems at greater depths and isolated by geological barriers, constitutes simultaneously a unique environmental archive and monument, therefore, it should be protected in a more rigorous way and rationally managed.

5

The Optical Gravitational Lensing Experiment. Search for Planetary and Low-Luminosity Object Transits in the Galactic Disk. Results of 2001 Campaign

Udalski A., Paczyński B., Żebruń K., Szymański M., Kubiak M., Soszyński I., Szewczyk O., Wyrzykowski Ł., Pietrzyński G.

Acta Astronomica

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2002

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Vol. 52, No. 1

1--37

EN

We present results of an extensive photometric search for planetary and low-luminosity object transits in the Galactic disk stars commencing the third phase of the Optical Gravitational Lensing Experiment - OGLE-III. Photometric observations of three fields in the direction of the Galactic center (800 epochs per field) were collected on 32 nights during time interval of 45 days. Out of the total of 5 million stars monitored, about 52 000 Galactic disk stars with photometry better than 1.5% were analyzed for flat-bottomed eclipses with the depth smaller than 0.08 mag. Altogether 46 stars with transiting low-luminosity objects were detected. For 42 of them multiple transits were observed, a total of 185, allowing orbital period determination. Transits in two objects: OGLE-TR-40 and OGLE-TR-10, with the radii ratio of about 0.14 and estimate of the radius of the companion 1.0-1.5 RJup, resemble the well known planetary transit in HD 209458. The sample was selected by the presence of apparent transits only, with no knowledge on any other properties. Hence, it is very well suited for general study of low-luminosity objects. The transiting objects may be Jupiters, brown dwarfs, or M dwarfs. Future determination of the amplitude of radial velocity changes will establish their masses, and will confirm or refute the reality of the so called "brown dwarf desert". The low-mass stellar companions will provide new data needed for the poorly known mass-radius relation for the lower main sequence. All photometric data are available to the astronomical community from the OGLE Internet archive.

6

A Possible Planetary Event OGLE-2002-BLG-055

Jaroszyński M., Paczyński B.

Acta Astronomica

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2002

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Vol. 52, No. 4

361--367

EN

The microlensing event OGLE-2002-BLG-055 has a single, but very reliable data point, deviating upward from a single source microlensing light curve by 0.6 mag. The simplest interpretation calls for a binary lens with a strong parallax effect and the mass ratio in the range of 0.01-0.001, putting the companion in the Jupiter mass range. Given only a single deviant point it is impossible to fit a unique model. We propose a modification of the OGLE observing strategy: instant verification of reality of future deviant points, followed by frequent time sampling, to make a unique model fit possible.

7

The Distance to the Magellanic Clouds

Paczyński B.

Acta Astronomica

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2001

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Vol. 51, No. 2

81--89

EN

The distance to the LMC and SMC is a subject of controversy, with the difference between the extreme values in distance moduli exceeding 0.5 mag. While currently the best calibrated method is based on red clump giants, and the near future improvement is most likely to come from detached eclipsing binaries, the ultimate goal is to have a purely geometrical determination. The best prospect will be to use relatively wide binary stars, for which spectroscopic orbits will be obtained with large ground based telescopes, and astrometric orbits will be obtained either with SIM, or with future ground based interferometers. A preliminary list of 25 candidate systems is presented. It is based on OGLE catalogs of BVI photometry.

8

Gamma-Ray Bursts at Low Redshift

Paczyński B.

Acta Astronomica

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2001

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Vol. 51, No. 1

1--4

EN

Long duration gamma-ray bursts (GRBs) are at cosmological distance, they appear to be located near star forming regions and are likely associated with some type of supernovae. They are also likely to be strongly beamed, which lowers their energetics by several orders of magnitude and increases their rate by the same factor. Therefore, it is likely that one out of 100-1000 core collapse supernovae generates ultra-relativistic jets, which beam gamma-rays and all other early emission into two narrow cones. After a year or so, the jets are decelerated, become non-relativistic and their emission becomes more or less isotropic. At least two GRBs: 970508 (z=0.835) and 980703 (z=0.966) show strong radio emission from late and therefore non-relativistic afterglows. Such events should be readily detectable at low redshift, say z=0.03. A search for strong radio emitters among recent nearby supernovae should be done about one year after the explosion. If some of these explosions generated GRBs and their gamma-ray beam missed us the bipolar structure of the radio remnant should be resolvable with VLBA.

9

Koncepcja rozwoju i zastosowań komputerowej Mapy hydrogeologicznej Polski w skali 1 : 50 000

Herbich P., Paczyński B., Płochniewski Z.

Przegląd Geologiczny

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2000

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Vol. 48, nr 6

495-497

10

Mapa Hydrogeologiczna Polski w skali 1:50 000 nowym etapem polskiej kartografii hydrogeologicznej

Paczyński B., Płochniewski Z., Sadurski A.

Biuletyn Państwowego Instytutu Geologicznego

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1999

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nr 388 Hydrogeologia

191-210

PL

Pierwsze mapy hydrogeologiczne terenów Polski powstały prawie sto lat temu. Jednak kartografia hydrogeologiczna jako oddzielna dyscyplina ukształtowała się w końcu lat trzydziestych. Powstał wówczas pierwszy arkusz Łódź, Mapy hydrogeologicznej Polski w skali 1:300 000. Kolejną mapę seryjną w skali 1:200 000 dla całego kraju opracowano w latach 1981-1988. W 1996 r. podjęto pracę nad komputerową Mapą hydrogeologiczną Polski w skali 1 : 50 000 (MhP). Nową generację mapy przygotowano w systemie GIS/INTERGRAPH. Wszystkie informacje geologiczne zestawione są w bazie danych systemu ORACLE, który powiązany jest z programem GEOMEDIA, umożliwiającym tworzenie map dla różnych potrzeb. MhP otwiera nowy etap polskiej kartografii.

EN

First hydrogeological map of Polish area was elaborated 100 years ago, but hydrogeological cartography as a separate discipline was established in late 30-ties. First sheet - Łódź, of Hydrogeological Map of Poland started at that time. This groundwater image was published in scale 1:300,000. More detail map in scale 1:200,000 was done in time 1981-1988. The computer Hydrogeological Map of Poland in scale 1:50,000 started in 1996 yr. It is a new generation map, preparing in GIS/INTERGRAPH system. All hydrogeological information collected in the ORACLE relational data base, together with GEOMEDIA program enables new specialized map creation according to an order from investor. This is also a new step in Polish hydrogeological cartography.

11

The Optical Gravitational Lensing Experiment. UBVI Photometry of Stars in Baade's Window

Paczyński B., Udalski A., Szymański M., Kubiak M., Pietrzyński G., Soszyński I., Woźniak P., Żebruń K.

Acta Astronomica

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1999

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Vol. 49, No. 3

319--339

EN

We present UBVI photometry for 8530 stars in Baade's Window obtained during the OGLE-II microlensing survey. Among these are over one thousand red clump giants. 1391 of them have photometry with errors smaller than 0.04, 0.06, 0.12, and 0.20 mag in the I, V, B, and U-band, respectively. We constructed a map of interstellar reddening. The corrected colors of the red clump giants: (U-B)0, (B-V)0, and (V-I)0 are very well correlated, indicating that a single parameter determines the observed spread of their values, reaching almost 2 mag in the (U-B)0. It seems most likely that heavy element content is the dominant parameter, but it is possible that another parameter: the age (or mass) of a star moves it along the same trajectory in the color-color diagram as the metallicity. The current ambiguity can be resolved with spectral analysis, and our catalog may be useful as a finding list of red clump giants. We point out that these K giants are more suitable for a fair determination of the distribution of metallicity than brighter M giants. We also present a compilation of UBVI data for 308 red clump giants near the Sun, for which Hipparcos parallaxes are more accurate than 10%. Spectral analysis of their metallicity may provide information about the local metallicity distribution as well as the extent to which mass (age) of these stars affects their colors. It is remarkable that in spite of a number of problems, stellar models agree with observations at the 0.1-0.2 mag level, making red clump giants not only the best calibrated but also the best understood standard candle.

12

Metallicity of Red Clump Giants in Baade's Window

Paczyński B.

Acta Astronomica

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1998

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Vol. 48, No. 3

405--412

EN

The red clump giants are potentially very useful as standard candles. There is some controversy about the stability of their I-band absolute magnitude, but it does not seem to be serious. No controversy was anticipated about their colors, with metal rich giants expected to be redder and cooler than the metal poor giants. The purpose of this paper is to point out that no such correlation is apparent between [Fe/H] and Teff as determined with Washington CCD photometry for the giants in Baade's Window. No explanation is offered for this surprising result. It is also unknown why the Galactic bulge red clump giants are redder than the clump giants near the Sun by 0.2 mag in the (V-I)0 color.

13

Advection Dominated Accretion Flows. A Toy Disk Model

Paczyński B.

Acta Astronomica

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1998

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Vol. 48, No. 4

667--676

EN

A toy model of a disk undergoing steady state accretion onto a black hole is presented. The disk is in a hydrostatic equilibrium for all radii r>rin, with the inner disk radius located between the marginally stable and marginally bound orbits: rms>rin>rmb. Matter flows from the disk through a narrow cusp at rms and falls freely into the black hole carrying with it no thermal energy. At radii larger than rout the disk is assumed to radiate away all locally generated heat, and therefore the disk is geometrically thin for r>rout. We assume that no heat generated in the inner disk, with rout>r>rin can be radiated away, i.e., the disk is 100% advective, and it becomes geometrically thick in this range of radii. All enthalpy of the thick disk is used up to press the inner disk radius towards the marginally bound orbit, and to lower the efficiency of conversion of accreted mass into radiation generated only for r>rout, by assumption. Conservation laws of mass, angular momentum and energy make it possible to calculate the inner thick disk radius rin for any specified value of its outer radius rout. As the nature of disk viscosity is not known there is some freedom in choosing the shape of the thick disk, subject to several general conditions which include the hydrostatic equilibrium everywhere for r>rin. The main purpose of this toy model is to emphasize the effect the disk thickness has on lowering the energetic efficiency of a black hole accretion.