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3. Approach of the NGC 1977 star cluster to the TOI-2796 host star

Author

Wakjira, Hawi Yohanis, Mosunova, D. A., Postnikova, E. S., Chupina, N. V., and Vereshchagin, S. V.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We study of possible encounters in past epochs of the open star cluster NGC 1977 with host stars. For this purpose, the age of the cluster was determined based on our catalog data. Stars with planetary systems were selected from the NASA Archive. The age of the cluster was determined using the color - absolute magnitude diagram and the isochron system. By extending the track of the movement of the cluster and stars in past epochs, 10 Myr. The time of the maximum approach 32 pc of the host star with planetary system TOI-2796 with the NGC 1977 are found. The place of approach in the sky is shown, this point can be considered as the place of appearance of interstellar comets. Thus, the result of our work is that the we found approach of the host star to the cluster entailed effects associated with the gravitational influence of the cluster on the nuclei of comets located in the outer parts of the Oort cloud of the planetary system. The effect of approach on comets is estimated.

Published
2023

6. Status and initial physics performance studies of the MPD experiment at NICA

Author

MPD Collaboration, Abgaryan, V., Kado, R. Acevedo, Afanasyev, S. V., Agakishiev, G. N., Alpatov, E., Altsybeev, G., Hernández, M. Alvarado, Andreeva, S. V., Andreeva, T. V., Andronov, E. V., Anfimov, N. V., Aparin, A. A., Astakhov, V. I., Atkin, E., Aushev, T., Averichev, G. S., Averyanov, A. V., Ayala, A., Babkin, V. A., Babutsidze, T., Balashov, I. A., Bancer, A., Barabanov, M. Yu., Baranov, D. A., Baranova, N., Barbashina, N., Baskakov, A. E., Batyuk, P. N., Bazhazhin, A. G., Baznat, D., Baznat, M., Bazylev, S. N., Beltran, L. G. E., Belyaev, A. V., Belyaev, S. E., Belyaeva, E. V., Benda, V., Bielewicz, M., Bietenholz, W., Blaschke, D., Blau, D., Bogdanova, G., Bogoslovsky, D. N., Boguslavsky, I. V., Boos, E., Botvina, A., Bravina, L., Bulychjov, S. A., Buryakov, M. G., Butenko, A. V., Butorin, A. V., Buzin, S. G., Bychkov, A., Bychkov, A. V., Cabellero, R. R., Arciniega, D. Chaires, Chalyshev, V. V., Chen, W., Chen, Z., Cheplakova, V. A., Chepurnov, V. F., Chepurnov, V. V., Cheremnova, M., Cheremukhina, G. A., Chlad, L., Chudoba, P., Chumakov, P. V., Cuautle, E., Czarnynoga, M., Dabrowska, B., Dąbrowski, D., Demanov, A., Dementyev, D. V., Deng, Z., Dmitriev, A. V., Dodokhov, V. Kh., Dolbilina, E. V., Dolbilov, A. G., Domínguez, I., Dominik, W., Donets, D. E., Dronik, V., Dubrovin, A. Yu., Dudziński, A., Dulov, P., Dunin, N. V., Dunin, V. B., Dyatlov, V., Dydyshko, V. F., Efremov, A. A., Egorov, D. S., Elsha, V. V., Emelyanov, A. E., Emelyanov, N. E., Ermakova, V. G., Eyyubova, G., Fang, D., Fateev, O. V., Fedin, O., Fedotov, Yu. I., Fedyunin, A. A., Feng, C., Feng, S., Feofilov, G. A., Filippov, I. A., Fischer, T., Formenko, K., Gaganova, M. A., Gandzhelashvili, T. T., Gavrishchuk, O. P., Geraksiev, N., Gerasimov, S. E., Gertsenberger, K. V., Golosov, O., Golovatyuk, V. M., Golubeva, M., Goncharov, I., Gorbunov, N. V., Grabowski, M., Grodzicka-Kobyłka, M., Grodzicki, K., Grzyb, J., Guber, F., Guirado, A., Guskov, A. V., Guzey, V., He, W., Rosas, L. A. Hernández, Huang, M., Huang, Y., Idczak, R., Idrisov, D., Igolkin, S. N., Ilieva, M., Isupov, A. Yu., Ivanishchev, D., Ivanov, A. V., Ivanytskyi, O., Ivashkin, A., Izvestnyy, A., Jaworska, E., Jiao, J., Kadochnikov, I., Kakurin, S. I., Kankiewicz, P., Kapishin, M. N., Karmanov, D., Karpushkin, N., Kartashova, L. A., Kashirin, E., Kasprowicz, G., Kasumov, Yu., Kechechyan, A. O., Kekelidze, G. D., Kekelidze, V. D., Khanzadeev, A., Kharlamov, P., Khilinova, O. A., Khodzhibagiyan, G. G., Khosravi, N., Khvorostukhin, A., Khyzhniak, Y., Kikvadze, V., Kireyeu, V. A., Kiryushin, Yu. T., Kiryutin, I. S., Kisiel, A., Klyuev, A., Klyukhin, V., Kochenda, L., Kodolova, O., Kolesnikov, V. I., Kolozhvari, A., Komarov, V. G., Kondratiev, V. P., Korolev, M., Korotkikh, V., Kotov, D., Kovalenko, S., Kovalenko, V. N., Kowalski, S., Kozlenko, N. A., Krakowiak, M., Kramarenko, V. A., Krasnova, L. M., Kravchov, P., Krechetov, Yu. F., Kruglova, I. V., Krylov, A. V., Krylov, V., Kryshen, E., Kryukov, A., Kubankin, A., Kugler, A., Kuich, M., Kukarnikov, S. I., Kuklin, S. N., Kukulin, V., Kuleshov, S., Kulikov, E. A., Kulikov, V. V., Kurepin, A., Kushpil, S., Kuzmin, V. S., Kvita, J., Lanskoy, D., Lashmanov, N. A., Ławryńczuk, M., Lazareva, T. V., Lednicky, R., Li, S., Li, Z., Litvinenko, A. G, Litvinenko, E. I., Litvinova, G. N., Liu, D., Liu, F., Livanov, A. N., Lobanov, V. I., Lobanov, Yu. Yu., Lobastov, S. P., Lokhtin, I., Lu, P., Lukstinsh, Yu. R., Luong, B. V., Łysakowski, B., Ma, Y., Machavariani, A., Madigozhin, D. T., Maksiak, B., Maksimenkova, V. I., Malakhov, A. I., Malayev, M., Maldonado, I., Maldonado, J. C., Malikov, I. V., Malinina, L., Maltsev, N. A., Maria, N. V., Shopova, M., Martemianov, M. A., Maslan, M., Matsyuk, M. A., Matulewicz, T., Melnikov, D. G., Merkin, M., Merts, S. P., Meshkov, I. N., Mianowski, S., Migulina, I. I., Mikhaylov, K. R., Milewicz-Zalewska, M., Minaev, Yu. I., Molokanova, N. A., Moreno-Barbosa, E., Morozov, S., Moshkin, A. A., Moshkovsky, I. V., Moskovsky, A. E., Movchan, S. A., Mudrokh, A. A., Mukhin, K. A., Murin, Yu. A., Musul'manbekov, Zh. Zh., Myalkovsky, V. V., Myktybekov, D., Paredes, L. L. Narvaez, Nauruzbaev, D. K., Nazarova, E. N., Nechaevsky, A. V., Nesterov, D. G., Nie, M., Nieto-Marín, P. A., Nigmatkulov, G., Nikitin, V. A., Nioradze, M., Niu, X., Nowak, W., Nozka, L., Oleks, I. A., Olshevsky, A. G., Orlov, O. E., Parfenov, P., Parzhitsky, S. S., Patiño, M. E., Pavlyukevich, V. A., Penkin, V. A., Peresedov, V. F., Peresunko, D., Peshekhonov, D. V., Petrov, V. A., Petrushanko, S., Petukhov, O., Piasecki, K., Pichugina, D. V., Piloyan, A., Pilyar, A. V., Piyadin, S. M., Plamowski, S., Platonova, M., Pluta, J., Potanina, A. E., Potrebenikov, Yu. K., Poźniak, K., Prokhorova, D. S., Prokofiev, N. A., Protoklitow, F., Prozorov, A., Pszczel, D., Puchkov, A. M, Pukhaeva, N., Puławski, S., Rakhmatullina, A. R., Herrera, L. F. Rebolledo, Reyna-Ortiz, V. Z., Riabov, V., Riabov, Yu., Ridinger, N. O., Rikhvitsky, V., Rodriguez-Cahuantzi, M., Rogachevsky, O. V., Rogov, V. Yu., Rokita, P., Romanenko, G., Romaniuk, R., Romanova, A., Rosłon, K., Rossler, T., Calderon, E. F. Rozas, Rufanov, I. A., Rumyantsev, M. M., Rustamov, A., Rybakov, A. A., Rybczyński, M., Rybka, D., Rymshina, A. A., Rzadkiewicz, J., Sadygov, Z. Ya. -O., Samsonov, V. A., Sandul, V. S., Sattarov, R., Savenkov, A. A., Schmidt, K., Seballos, S. S., Sedykh, S. A., Selyuzhenkov, I., Semchukova, T. V., Semenov, A. Yu., Semenova, I. A., Sergeev, S. V., Sergeeva, N. A., Serochkin, E. V., Seryakov, A. Yu., Shabunov, A. V., Shanidze, R., Shcheglova, L., Shchinov, B. G., Shen, C., Shen, Y., Sherbakov, A. N., Sheremetyev, A. D., Sheremetyeva, A. I., Shindin, R. A., Shipunov, A. V., Shitenkov, M. O., Shtejer, D. K., Shukla, U., Shunko, A. A., Shutov, A. V., Shutov, V. B., Sidorin, A. O., Skwira-Chalot, I., Slepnev, I. V., Slepnev, V. M., Slepov, I. P., Solnyshkin, Yu. A., Solomin, A., Solovyeva, T., Sorin, A. S., Starecki, T., Stefanek, G., Stepaniak, J., Streletskaya, E. A., Strikhanov, M., Strizh, T. A., Strizhak, A., Sukhov, N. V., Sukhovarov, S. I., Sun, X., Surkov, N. N., Suvarieva, D., Svalov, V. L., Świderski, L., Syntfeld-Każuch, A., Szcześniak, T., Szewiński, J., Tang, Z., Taranenko, A., Tarasov, N. A., Tcholakov, V., Tejeda-Muñoz, G., Tejeda-Yeomans, M. E., Terletskiy, A. V., Teryaev, O. V., Tikhomirov, V. V., Timoshenko, A. A., Tkachev, G. P., Toneev, V. D., Topilin, N. D., Traczyk, T., Tretyakova, T., Trubnikov, A. V., Trubnikov, G. V., Tyapkin, I. A., Udovenko, S. Yu., Poblete, P. A. Ulloa, Urbaniak, M., Urumov, V., Valenzuela-Cazares, L., Valiev, F. F., Vasendina, V. A., Vasiliev, I. N., Vasilyev, A., Vechernin, V. V., Vereshchagin, S. V., Vladimirova, N. N., Vlasov, N. V., Vodopyanov, A. S., Vokhmyanina, K., Volkov, V., Volodina, O. A., Voronin, A. A., Voronyuk, V., Wang, F., Wang, J., Wang, X., Wang, Y., Wieczorek, P., Wielanek, D., Włodarczyk, Z., Wójcik, K., Wu, K., Xiao, Z., Xu, Q., Yang, C., Yang, H., Yang, Q., Yarygin, G. A., Yordanova, L., Yu, T., Yuan, Z., Yurevich, V. I., Zabołotny, W., Zabrodin, E., Zaitseva, M. V., Saa, J. A. Zamora, Zamyatin, N. I., Zaporozhets, S. A., Zarochentsev, A. K., Zepeda-Fernández, C. H., Zha, W., Zhalov, M., Zhang, Y., Zhang, Z., Zhao, C., Zherebchevsky, V. I., Zhezher, V. N., Zhong, C., Zhou, W., Zhu, X., Zinchenko, A. I., and Zinchenko, D. A.

Subjects
Physics - Instrumentation and Detectors, High Energy Physics - Experiment, Nuclear Experiment, Nuclear Theory
Abstract

The Nuclotron-base Ion Collider fAcility (NICA) is under construction at the Joint Institute for Nuclear Research (JINR), with commissioning of the facility expected in late 2022. The Multi-Purpose Detector (MPD) has been designed to operate at NICA and its components are currently in production. The detector is expected to be ready for data taking with the first beams from NICA. This document provides an overview of the landscape of the investigation of the QCD phase diagram in the region of maximum baryonic density, where NICA and MPD will be able to provide significant and unique input. It also provides a detailed description of the MPD set-up, including its various subsystems as well as its support and computing infrastructures. Selected performance studies for particular physics measurements at MPD are presented and discussed in the context of existing data and theoretical expectations., Comment: 53 pages, 68 figures, submitted as a Review article to EPJA

Published
2022
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7. A Gaia based photometric and kinematic analysis of the old open cluster King 11

Author

Sariya, Devesh P., Jiang, Ing-Guey, Bisht, D., Sizova, M. D., Chupina, N. V., Vereshchagin, S. V., Yadav, R. K. S., and Rangwal, G.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

This paper presents an investigation of an old age open cluster King 11 using Gaia's Early Data Release 3 (EDR3) data. Considering the stars with membership probability ($P_{\mu}$) $> 90\%$, we identified 676 most probable cluster members within the cluster's limiting radius. The mean proper motion (PM) for King 11 is determined as: $\mu_{x}=-3.391\pm0.006$ and $\mu_{y}=-0.660\pm0.004$ mas yr$^{-1}$. The blue straggler stars (BSS) of King 11 show a centrally concentrated radial distribution. The values of limiting radius, age, and distance are determined as 18.51 arcmin, 3.63$\pm$0.42 Gyr and $3.33\pm0.15$ kpc, respectively. The cluster's apex coordinates ($A=267.84^{\circ} \pm 1.01^{\circ}$, $D=-27.48^{\circ} \pm 1.03^{\circ}$) are determined using the apex diagram (AD) method and verified using the ($\mu_U$,$\mu_T$) diagram. We also obtained the orbit that the cluster follows in the Galaxy and estimated its tentative birthplace in the disk. The resulting spatial velocity of King 11 is 60.2 $\pm$ 2.16 km s$^{-1}$. A significant oscillation along the $Z$-coordinate up to 0.556$\pm$0.022~kpc is determined.

Published
2021
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8. A comprehensive analysis of NGC 2158 in Gaia era: photometric parameters, apex and orbit

Author

Sariya, Devesh P., Jiang, Ing-Guey, Sizova, M. D., Postnikova, E. S., Bisht, D., Chupina, N. V., Vereshchagin, S. V., Yadav, R. K. S., Rangwal, G., and Tutukov, A. V.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present an investigation of NGC 2158 using Gaia-DR2 data. We identified 800 most likely cluster members with membership probability higher than 90%. The mean proper motions of this object are determined as (mu_{x}=-0.203 \pm 0.003, mu_{y}=-1.99 \pm 0.004) mas yr^{-1}. The limiting radius, log(age), and distance of the cluster are obtained as 23.5 arcmin, 9.38 \pm 0.04 Gyr and 4.69 \pm 0.22 kpc, respectively. The overall mass function slope (0.93 \pm 0.14) is flatter than the Salpeter value (1.35) within the mass range 1.17-1.44 M_\odot. This cluster also shows the mass-segregation effect and our study demonstrates that NGC 2158 is a dynamically relaxed open cluster. Using the AD-diagram, the apex coordinates of the cluster are obtained in different ways and examined using (\mu_{U},\mu_{T}) diagram. The best value of apex coordinates is determined as A=87.24^\circ \pm 1.60^\circ, D=-36.61^\circ \pm 5.30 ^\circ. We also determined the orbit of the cluster and found that NGC 2158 moves almost in the Solar antapex direction. The resulting spatial velocity of NGC 2158 is 51 km s^{-1}. A significant oscillations along the Z-coordinate up to 529~pc is detected. Various scenarios regarding the origin of this cluster are also discussed., Comment: 36 pages, 15 figures. Original submission on 25th June 2020 and accepted for the publication by The Astronomical Journal (AJ) on 10th December 2020

Published
2020
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10. Hyades star cluster and the New comets

Author

Sizova, M. D., Postnikova, E. S., Demidov, A. P., Chupina, N. V., and Vereshchagin, S. V.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

We examined the influence of the Hyades star cluster on the possibility of the appearance of long-period comets in the Solar system. It is known that the Hyades cluster is extended along the spatial orbit on tens of parsecs. To our estimations, 0.85 million years ago, there was a close approach of the cluster to the Sun of 24.8 pc. The approach of one of the cluster stars to the Sun at the minimally known distance of about 6.9 pc was 1.6 million years ago. The main part of the cluster was close to the Sun from 1 to 2 million years ago. Such proximity is not essential for the impact on the dynamics of small bodies in the external part of the Oort cloud, although the view may change after additional study of the cluster structure. Possible orbits perihelion displacements of the small bodies of the outer part of the Oort cloud make some of them in observable comets region., Comment: Proceedings 49-th International student's conferences "Physics of Space", Kourovka, Ural Federal University (UrFU), 2020

Published
2019

11. The kinematical and space structures of IC 2391 open cluster and moving group with Gaia-DR2

Author

Postnikova, E. S., Elsanhoury, W. H., Sariya, Devesh P., Chupina, N. V., Vereshchagin, S. V., and Jiang, Ing-Guey

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The kinematical parameters, spatial shape and structure of the open cluster IC 2391 and the associated stellar stream are studied here using Gaia-DR2 (GDR2) astrometry data. The apex positions are determined for the open cluster IC 2391 (data taken from Cantat-Gaudin et al.) and for the kinematical streams stars mentioned in Montes et al. using both convergent point and AD-diagram methods. The values of apex coordinates identified. The results are in good agreement with the previously calculated values. The positions of the stars in the disk and the spatial dispersion velocities are determined. The paths of cluster and associated stream are traced in the disk by orbit calculation back in time to their places of formation. A possible genetic relationship between the cluster and the stream has been detected. The approximation of the spatial and kinematical shape of the stream and the cluster is made. According to this study, even though currently the cluster and the stream seem to have spatial difference in their locations but they appear to have formed in the same region of the Galactic disk.

Published
2019
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13. The Pleiades apex and its kinematical structure

Author

Elsanhoury, W. H., Postnikova, E. S., Chupina, N. V., Vereshchagin, S. V., Sariya, Devesh P., Yadav, R. K. S., and Jiang, Ing-Guey

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

A study of cluster characteristics and internal kinematical structure of the middle-aged Pleiades open star cluster is presented. The individual star apexes and various cluster kinematical parameters including the velocity ellipsoid parameters are determined using both Hipparcos and Gaia data. Modern astrometric parameters were taken from the Gaia Data Release 1 (DR1) in combination with the Radial Velocity Experiment Fifth Data Release (DR5). The necessary set of parameters including parallaxes, proper motions and radial velocities are used for n=17 stars from Gaia DR1+RAVE DR5 and for n=19 stars from the Hipparcos catalog using SIMBAD data base. Single stars are used to improve accuracy by eliminating orbital movements. RAVE DR5 measurements were taken only for the stars with the radial velocity errors not exceeding $2$~km/s. For the Pleiades stars taken from Gaia, we found mean heliocentric distance as $136.8 \pm 6.4$~pc, and the apex position is calculated as: $A_{CP}=92^\circ.52\pm1^\circ.72$, $D_{CP}=-42^\circ.28\pm2^\circ.56$ by the convergent point method and $A_0=95^\circ.59\pm2^\circ.30$ and $D_0=-50^\circ.90\pm2^\circ.04$ using AD-diagram method (n=17 in both cases). The results are compared with those obtained historically before the Gaia mission era., Comment: 2 Figures, 4 Tables, Accepted for publication in Astrophysics and Space Science

Published
2018
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14. Radial velocity dispersions of star groups in M 67

Author

Vereshchagin, S. V. and Chupina, N. V.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

High-precision measurements of radial velocities of the M 67 cluster members are used to calculate the radial-velocity dispersions in the stellar groups found earlier in the cluster's corona. The previously detected feature in one of the groups (Group 60) consisting of stars with almost identical space velocities was confirmed. The possibility of more accurate future studies of the parameters of star groups using the Gaia catalogues is discussed., Comment: 7 pages, 2 figures

Published
2017

16. 2MASS photometry and kinematical studies of open cluster NGC 188

Author

Elsanhoury, W. H., Haroon, A. A., Chupina, N. V., Vereshchagin, S. V., Sariya, Devesh P., Yadav, R. K. S., and Jiang, Ing-Guey

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

In this paper, we present our results for the photometric and kinematical studies of old open cluster NGC 188. We determined various astrophysical parameters like limited radius, core and tidal radii, distance, luminosity and mass functions, total mass, relaxation time etc. for the cluster using 2MASS catalog. We obtained the cluster's distance from the Sun as 1721+/-41 pc and log (age)= 9.85+/-0.05 at Solar metallicity. The relaxation time of the cluster is smaller than the estimated cluster age which suggests that the cluster is dynamically relaxed. Our results agree with the values mentioned in the literature. We also determined the cluster's apex coordinates as (281.88 deg, -44.76 deg) using AD-diagram method. Other kinematical parameters like space velocity components, cluster center and elements of Solar motion etc. have also been computed., Comment: Accepted for publication in New Astronomy 5 Figures, 2 Tables

Published
2016
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17. Details of the spatial structure and kinematics of the Castor and Ursa Major streams

Author

Vereshchagin, S. V. and Chupina, N. V.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

A list of the Castor stream members is compiled based on the data from various authors. The membership probabilities for some stars are revised based on the individual apex, multiplicity, observational errors, and peculiarity. The apex of the Castor moving group is determined using the apex diagram method. The parameters of the Castor and Ursa Major streams are compared and the positions of the two streams on the apex diagram are found to differ by 225deg, implying that the two groups move in almost opposite directions. Stars of both moving groups are intermixed in space, the Castor stream occupies a smaller volume than the UMa stream and is located inside it. Our results can be useful for understanding the morphology of the Galactic disk in the Sun's vicinity.

Published
2016
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21. Apex determination and detection of stellar clumps in the open cluster M 67

Author

Vereshchagin, S. V., Chupina, N. V., Sariya, Devesh P., Yadav, R. K. S., and Kumar, Brijesh

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We determined the cluster apex coordinates, studied the substructures and performed membership analysis in the central part (34'X33') of the open cluster M 67. We used the individual stellar apexes method developed earlier and classical technique of proper motion diagrams in coordinate system connected with apex. The neighbour-to-neighbour distance technique was applied to detect space details. The membership list was corrected and some stars were excluded from the most probable members list. The apex coordinates have been determined as: A0=132.97deg+/-0.81deg and D0=11.85deg+/-0.90deg. The 2D-space star density field was analysed and high degree of inhomogeneity was found., Comment: 20 Pages, 8 Figures, 7 Tables Accepted for publication to New Astronomy

Published
2014
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27. Radial Velocity Dispersions of Star Groups in M67

Author

Vereshchagin S. V. and Chupina N. V.

Subjects
solar neighborhood, open clusters and associations: individual (m 67), Astronomy, QB1-991
Abstract

High-precision measurements of radial velocities of the M67 cluster members are used to calculate the radial-velocity dispersions in the stellar groups found earlier in the cluster’s corona. The previously detected feature in one of the groups (Group 60) consisting of stars with almost identical space velocities was confirmed. The possibility of more accurate future studies of the parameters of star groups using the Gaia catalogues is discussed.

Published
2016
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29. Digital Archive of the Astrograph Plates Stored at the Inasan Zvenigorod Observatory

Author

Vereshchagin S. V. and Chupina N. V.

Subjects
astronomical databases, techniques, digitizing, asteroids, comets, Astronomy, QB1-991
Abstract

The plate collection of the Zvenigorod 40-cm Carl Zeiss astrograph, obtained in 1972-2003, contains direct photographs of star fields, comets, asteroids, Pluto, and Mars. The electronic library of images from photographic plates was created from scanning the astronomical negatives. We present information on programs scheduled at the telescope and the structure and maintenance of the plate stacks. We also list the plates with images of asteroids and comets. Access to all our plate lists is provided at the web sites of the Institute of Astronomy (INASAN) and WFPDB. It is possible to select plates by the date of observation, by the coordinates of the sky area, by the object type. Preview images can be inspected.

Published
2012
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38. Searching for close approaches of the stars pairs in the galactic disk with Gaia EDR3 data

Author

Sizova, M. D. and Vereshchagin, S. V.

Abstract

С помощью расчетов орбит звезд вокруг центра Галактики проведен поиск пар звезд, сближавшихся на интервале 5 млн лет как в прошлые, так и в будущие эпохи. Найдены пары звезд, минимальное расстояние между которыми может составлять менее 1 пк. Рассмотренный процесс важен для изучения происхождения межзвездных комет. Using calculations of the orbital motion around the Galactic center we searched for approaching stars on 5 Myr in the past and the future. We provide stars that approached up to 1 pc to each other. Considered process is important for researching the interstellar small bodies origin. В этом исследовании использовалась база данных SIMBAD, CDS, Страсбург, Франция, «Астрономическая база данных SIMBAD» [12], а также данные ESA миссии Gaia (https://www.cosmos.esa.int/gaia), представленные Gaia DPAC https://www.cosmos.esa.int/web/gaia/dpac/consortium). Авторы благодарны за полезные советы Дж. Бови из Департамента астрономии и астрофизики Университета Торонто, в частности, об использовании пакета galpy, и А. В. Тутукову за полезные обсуждения и советы. Авторы благодарны рецензенту за полезные замечания.

Published
2021

41. Поиск близких сближений звезд в галактическом диске по данным Gaia EDR3

Author

Сизова, М. Д., Верещагин, С. В., Sizova, M. D., Vereshchagin, S. V., Сизова, М. Д., Верещагин, С. В., Sizova, M. D., and Vereshchagin, S. V.

Abstract

С помощью расчетов орбит звезд вокруг центра Галактики проведен поиск пар звезд, сближавшихся на интервале 5 млн лет как в прошлые, так и в будущие эпохи. Найдены пары звезд, минимальное расстояние между которыми может составлять менее 1 пк. Рассмотренный процесс важен для изучения происхождения межзвездных комет., Using calculations of the orbital motion around the Galactic center we searched for approaching stars on 5 Myr in the past and the future. We provide stars that approached up to 1 pc to each other. Considered process is important for researching the interstellar small bodies origin.

Published
2021

46. Hyades Star Cluster and a New Comets

Author

Sizova, M. D., Postnikova, E. S., Demidov, A. P., Chupina, N. V., and Vereshchagin, S. V.

Abstract

The Gaia DR2 data revealed that the Hyades star cluster is stretched along the spatial orbit for tens of parsecs. According to our estimates, 0.85 million years ago there was an approach of the cluster with the Sun up to 24.8 pc. The displacements of the perihelions of small bodies orbits in the outer Oort cloud turned them into observable comets. Известно, что скопление Гиады растянуто вдоль пространственной орбиты на десятки парсек. По нашим оценкам, 0.85 млн лет назад было сближение скопления с Солнцем до 24.8 пк. Возможные смещения перигелия орбит малых тел в облаке Оорта делают часть из них наблюдаемыми кометами. РаботаМ. Д. Сизовой частично поддержана Российским научным фондом (РНФ, 17-12-01441).

Published
2020

47. Звездное скопление Гиады и новые кометы

Author

Sizova, M. D., Postnikova, E. S., Demidov, A. P., Chupina, N. V., Vereshchagin, S. V., Сизова, М. Д., Постникова, Е. С., Демидов, А. П., Чупина, Н. В., Верещагин, С. В., Sizova, M. D., Postnikova, E. S., Demidov, A. P., Chupina, N. V., Vereshchagin, S. V., Сизова, М. Д., Постникова, Е. С., Демидов, А. П., Чупина, Н. В., and Верещагин, С. В.

Abstract

The Gaia DR2 data revealed that the Hyades star cluster is stretched along the spatial orbit for tens of parsecs. According to our estimates, 0.85 million years ago there was an approach of the cluster with the Sun up to 24.8 pc. The displacements of the perihelions of small bodies orbits in the outer Oort cloud turned them into observable comets., Известно, что скопление Гиады растянуто вдоль пространственной орбиты на десятки парсек. По нашим оценкам, 0.85 млн лет назад было сближение скопления с Солнцем до 24.8 пк. Возможные смещения перигелия орбит малых тел в облаке Оорта делают часть из них наблюдаемыми кометами.

Published
2020

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