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Your search keyword '"Suleimanov, V"' showing total 22 results
Start Over Author "Suleimanov, V" Publisher oxford university press (oup)
22 results on '"Suleimanov, V"'

2. X-ray polarimetry of X-ray pulsar X Persei: another orthogonal rotator?

Author

Mushtukov, A A, primary, Tsygankov, S S, additional, Poutanen, J, additional, Doroshenko, V, additional, Salganik, A, additional, Costa, E, additional, Marco, A Di, additional, Heyl, J, additional, Monaca, F La, additional, Lutovinov, A A, additional, Mereminsky, I A, additional, Papitto, A, additional, Semena, A N, additional, Shtykovsky, A E, additional, Suleimanov, V F, additional, Forsblom, S V, additional, González-Caniulef, D, additional, Malacaria, C, additional, Sunyaev, R A, additional, Agudo, I, additional, Antonelli, L A, additional, Bachetti, M, additional, Baldini, L, additional, Baumgartner, W H, additional, Bellazzini, R, additional, Bianchi, S, additional, Bongiorno, S D, additional, Bonino, R, additional, Brez, A, additional, Bucciantini, N, additional, Capitanio, F, additional, Castellano, S, additional, Cavazzuti, E, additional, Chen, C-T, additional, Ciprini, S, additional, De Rosa, A, additional, Del Monte, E, additional, Gesu, L Di, additional, Lalla, N Di, additional, Donnarumma, I, additional, Dovčiak, M, additional, Ehlert, S R, additional, Enoto, T, additional, Evangelista, Y, additional, Fabiani, S, additional, Ferrazzoli, R, additional, Garcia, J A, additional, Gunji, S, additional, Hayashida, K, additional, Iwakiri, W, additional, Jorstad, S G, additional, Kaaret, P, additional, Karas, V, additional, Kislat, F, additional, Kitaguchi, T, additional, Kolodziejczak, J J, additional, Krawczynski, H, additional, Latronico, L, additional, Liodakis, I, additional, Maldera, S, additional, Manfreda, A, additional, Marin, F, additional, Marscher, A P, additional, Marshall, H L, additional, Massaro, F, additional, Matt, G, additional, Mitsuishi, I, additional, Mizuno, T, additional, Muleri, F, additional, Negro, M, additional, Ng, C-Y, additional, O’Dell, S L, additional, Omodei, N, additional, Oppedisano, C, additional, Pavlov, G G, additional, Peirson, A L, additional, Perri, M, additional, Pesce-Rollins, M, additional, Petrucci, P-O, additional, Pilia, M, additional, Possenti, A, additional, Puccetti, S, additional, Ramsey, B D, additional, Rankin, J, additional, Ratheesh, A, additional, Roberts, O J, additional, Romani, R W, additional, Sgrò, C, additional, Slane, P, additional, Soffitta, P, additional, Spandre, G, additional, Swartz, D A, additional, Tamagawa, T, additional, Tavecchio, F, additional, Taverna, R, additional, Tawara, Y, additional, Tennant, A F, additional, Thomas, N E, additional, Tombesi, F, additional, Trois, A, additional, Turolla, R, additional, Vink, J, additional, Weisskopf, M C, additional, Wu, K, additional, Xie, F, additional, and Zane, S, additional

Published
2023
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5. X-ray reprocessing in accreting pulsar GX 301-2 observed with Insight-HXMT

Author

Ji, L, primary, Doroshenko, V, additional, Suleimanov, V, additional, Santangelo, A, additional, Orlandini, M, additional, Liu, J, additional, Ducci, L, additional, Zhang, S N, additional, Nabizadeh, A, additional, Gavran, D, additional, Zhang, S, additional, Ge, M Y, additional, Li, X B, additional, Tao, L, additional, Bu, Q C, additional, Qu, J L, additional, Lu, F J, additional, Chen, L, additional, Song, L M, additional, Li, T P, additional, Xu, Y P, additional, Cao, X L, additional, Chen, Y, additional, Liu, C Z, additional, Cai, C, additional, Chang, Z, additional, Chen, T X, additional, Chen, Y P, additional, Cui, W W, additional, Du, Y Y, additional, Gao, G H, additional, Gao, H, additional, Gu, Y D, additional, Guan, J, additional, Guo, C C, additional, Han, D W, additional, Huang, Y, additional, Huo, J, additional, Jia, S M, additional, Jiang, W C, additional, Jin, J, additional, Kong, L D, additional, Li, B, additional, Li, C K, additional, Li, G, additional, Li, W, additional, Li, X, additional, Li, X F, additional, Li, Z W, additional, Liang, X H, additional, Liao, J Y, additional, Liu, B S, additional, Liu, H X, additional, Liu, H W, additional, Liu, X J, additional, Lu, X F, additional, Luo, Q, additional, Luo, T, additional, Ma, R C, additional, Ma, X, additional, Meng, B, additional, Nang, Y, additional, Nie, J Y, additional, Ou, G, additional, Ren, X Q, additional, Sai, N, additional, Song, X Y, additional, Sun, L, additional, Tan, Y, additional, Tuo, Y L, additional, Wang, C, additional, Wang, L J, additional, Wang, P J, additional, Wang, W S, additional, Wang, Y S, additional, Wen, X Y, additional, Wu, B Y, additional, Wu, B B, additional, Wu, M, additional, Xiao, G C, additional, Xiao, S, additional, Xiong, S L, additional, Yang, R J, additional, Yang, S, additional, Yang, Yan-Ji, additional, Yang, Yi-Jung, additional, Yi, Q B, additional, Yin, Q Q, additional, You, Y, additional, Zhang, F, additional, Zhang, H M, additional, Zhang, J, additional, Zhang, P, additional, Zhang, W, additional, Zhang, W C, additional, Zhang, Yi, additional, Zhang, Y F, additional, Zhang, Y H, additional, Zhao, H S, additional, Zhao, X F, additional, Zheng, S J, additional, Zheng, Y G, additional, and Zhou, D K, additional

Published
2020
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6. Measuring the masses of magnetic white dwarfs: a NuSTAR legacy survey

Author

Shaw, A W, primary, Heinke, C O, additional, Mukai, K, additional, Tomsick, J A, additional, Doroshenko, V, additional, Suleimanov, V F, additional, Buisson, D J K, additional, Gandhi, P, additional, Grefenstette, B W, additional, Hare, J, additional, Jiang, J, additional, Ludlam, R M, additional, Rana, V, additional, and Sivakoff, G R, additional

Published
2020
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7. Switches between accretion structures during flares in 4U 1901+03

Author

Ji, L, primary, Ducci, L, primary, Santangelo, A, primary, Zhang, S, primary, Suleimanov, V, primary, Tsygankov, S, primary, Doroshenko, V, primary, Nabizadeh, A, primary, Zhang, S N, primary, Ge, M Y, primary, Tao, L, primary, Bu, Q C, primary, Qu, J L, primary, Lu, F J, primary, Chen, L, primary, Song, L M, primary, Li, T P, primary, Xu, Y P, primary, Cao, X L, primary, Chen, Y, primary, Liu, C Z, primary, Cai, C, primary, Chang, Z, primary, Chen, G, primary, Chen, T X, primary, Chen, Y B, primary, Chen, Y P, primary, Cui, W, primary, Cui, W W, primary, Deng, J K, primary, Dong, Y W, primary, Du, Y Y, primary, Fu, M X, primary, Gao, G H, primary, Gao, H, primary, Gao, M, primary, Gu, Y D, primary, Guan, J, primary, Guo, C C, primary, Han, D W, primary, Huang, Y, primary, Huo, J, primary, Jia, S M, primary, Jiang, L H, primary, Jiang, W C, primary, Jin, J, primary, Jin, Y J, primary, Kong, L D, primary, Li, B, primary, Li, C K, primary, Li, G, primary, Li, M S, primary, Li, W, primary, Li, X, primary, Li, X B, primary, Li, X F, primary, Li, Y G, primary, Li, Z W, primary, Liang, X H, primary, Liao, J Y, primary, Liu, B S, primary, Liu, G Q, primary, Liu, H X, primary, Liu, H W, primary, Liu, X J, primary, Liu, Y N, primary, Lu, B, primary, Lu, X F, primary, Luo, Q, primary, Luo, T, primary, Ma, X, primary, Meng, B, primary, Nang, Y, primary, Nie, J Y, primary, Ou, G, primary, Sai, N, primary, Shang, R C, primary, Song, X Y, primary, Sun, L, primary, Tan, Y, primary, Tuo, Y L, primary, Wang, C, primary, Wang, G F, primary, Wang, J, primary, Wang, P J, primary, Wang, W S, primary, Wang, Y S, primary, Wen, X Y, primary, Wu, B Y, primary, Wu, B B, primary, Wu, M, primary, Xiao, G C, primary, Xiao, S, primary, Xiong, S L, primary, Xu, H, primary, Yang, J W, primary, Yang, S, primary, Yang, Yan-Ji, primary, Yang, Yi-Jung, primary, Yi, Q B, primary, Yin, Q Q, primary, You, Y, primary, Zhang, A M, primary, Zhang, C M, primary, Zhang, F, primary, Zhang, H M, primary, Zhang, J, primary, Zhang, P, primary, Zhang, T, primary, Zhang, W, primary, Zhang, W C, primary, Zhang, W Z, primary, Zhang, Yi, primary, Zhang, Y F, primary, Zhang, Y J, primary, Zhang, Y H, primary, Zhang, Yue, primary, Zhang, Zhao, primary, Zhang, Zhi, primary, Zhang, Z L, primary, Zhao, H S, primary, Zhao, X F, primary, Zheng, S J, primary, Zhou, D K, primary, Zhou, J F, primary, Zhu, Y X, primary, Zhu, Y, primary, and Zhuang, R L, primary

Published
2020
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9. From outburst to quiescence: spectroscopic evolution of V1838 Aql imbedded in a bow-shock nebula

Author

Santisteban, J V Hernández, primary, Echevarría, J, additional, Zharikov, S, additional, Neustroev, V, additional, Tovmassian, G, additional, Chavushyan, V, additional, Napiwotzki, R, additional, R, Costero, additional, Michel, R, additional, Sánchez, L J, additional, Ruelas–Mayorga, A, additional, Olguín, L, additional, García–Díaz, Ma T, additional, González–Buitrago, D, additional, de Miguel, E, additional, de la Fuente, E, additional, de Anda, R, additional, and Suleimanov, V, additional

Published
2019
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10. The remarkable outburst of the highly-evolved post period-minimum dwarf nova SSS J122221.7−311525

Author

Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Neustroev, V. V., Marsh, T. R., Zharikov, S. V., Knigge, C., Kuulkers, E., Osborne, J. P., Page, K. L., Steeghs, D., Suleimanov, V. F., Tovmassian, G., Breedt, E., Frebel, Anna L., García-Díaz, Ma. T., Hambsch, F.-J., Jacobson, Heather, Parsons, S. G., Ryu, T., Sabin, L., Sjoberg, G., Miroshnichenko, A. S., Reichart, D. E., Haislip, J. B., Ivarsen, K. M., LaCluyze, A. P., Moore, J. P., Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Neustroev, V. V., Marsh, T. R., Zharikov, S. V., Knigge, C., Kuulkers, E., Osborne, J. P., Page, K. L., Steeghs, D., Suleimanov, V. F., Tovmassian, G., Breedt, E., Frebel, Anna L., García-Díaz, Ma. T., Hambsch, F.-J., Jacobson, Heather, Parsons, S. G., Ryu, T., Sabin, L., Sjoberg, G., Miroshnichenko, A. S., Reichart, D. E., Haislip, J. B., Ivarsen, K. M., LaCluyze, A. P., and Moore, J. P.

Abstract

We report extensive 3-yr multiwavelength observations of the WZ Sge-type dwarf nova SSS J122221.7-311525 during its unusual double superoutburst, the following decline and in quiescence. The second segment of the superoutburst had a long duration of 33 d and a very gentle decline with a rate of 0.02 mag d-1, and it displayed an extended post-outburst decline lasting at least 500 d. Simultaneously with the start of the rapid fading from the superoutburst plateau, the system showed the appearance of a strong near-infrared excess resulting in very red colours, which reached extreme values (B - I ≃ 1.4) about 20 d later. The colours then became bluer again, but it took at least 250 d to acquire a stable level. Superhumps were clearly visible in the light curve from our very first time-resolved observations until at least 420 d after the rapid fading from the superoutburst. The spectroscopic and photometric data revealed an orbital period of 109.80 min and a fractional superhump period excess ≲0.8 per cent, indicating a very low mass ratio q ≲ 0.045. With such a small mass ratio the donor mass should be below the hydrogen-burning minimum mass limit. The observed infrared flux in quiescence is indeed much lower than is expected from a cataclysmic variable with a nearmain- sequence donor star. This strongly suggests a brown-dwarf-like nature for the donor and that SSS J122221.7-311525 has already evolved away from the period minimum towards longer periods, with the donor now extremely dim. Keywords: binaries: close; stars: evolution; stars: individual: SSS J122221.7−311525; novae; cataclysmic variables

Published
2019

14. Detection of burning ashes from thermonuclear X-ray bursts

Author

Kajava, J. J. E., Nättilä, Joonas, Poutanen, Juri, Cumming, A., Suleimanov, V., Kuulkers, E., Kajava, J. J. E., Nättilä, Joonas, Poutanen, Juri, Cumming, A., Suleimanov, V., and Kuulkers, E.

Abstract

When neutron stars (NS) accrete gas from low-mass binary companions, explosive nuclear burning reactions in the NS envelope fuse hydrogen and helium into heavier elements. The resulting thermonuclear (type-I) X-ray bursts produce energy spectra that are fit well with black bodies, but a significant number of burst observations show deviations from Planck spectra. Here we present our analysis of RXTE/ PCA observations of X-ray bursts from the NS low-mass X-ray binary HETE J1900.1-2455. We have discovered that the non-Planckian spectra are caused by photoionization edges. The anticorrelation between the strength of the edges and the colour temperature suggests that the edges are produced by the nuclear burning ashes that have been transported upwards by convection and become exposed at the photosphere. The atmosphere model fits show that occasionally the photosphere can consist entirely of metals, and that the peculiar changes in blackbody temperature and radius can be attributed to the emergence and disappearance of metals in the photosphere. As the metals are detected already in the Eddington-limited phase, it is possible that a radiatively driven wind ejects some of the burning ashes into the interstellar space., QC 20220329

Published
2017
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15. The remarkable outburst of the highly-evolved post period-minimum dwarf nova SSS J122221.7−311525

Author

Neustroev, V. V., primary, Marsh, T. R., additional, Zharikov, S. V., additional, Knigge, C., additional, Kuulkers, E., additional, Osborne, J. P., additional, Page, K. L., additional, Steeghs, D., additional, Suleimanov, V. F., additional, Tovmassian, G., additional, Breedt, E., additional, Frebel, A., additional, García-Díaz, Ma. T., additional, Hambsch, F.-J., additional, Jacobson, H., additional, Parsons, S. G., additional, Ryu, T., additional, Sabin, L., additional, Sjoberg, G., additional, Miroshnichenko, A. S., additional, Reichart, D. E., additional, Haislip, J. B., additional, Ivarsen, K. M., additional, LaCluyze, A. P., additional, and Moore, J. P., additional

Published
2017
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17. Dark spot, spiral waves and the sw sextantis behaviour: it is all about ux ursae majoris

Author

Neustroev, V. V., Suleimanov, V. F., Borisov, N. V., Belyakov, K. V., and Shearer, A.

Subjects
binaries: close, cataclysmic variables, doppler tomography, stationary accretion disks, Astrophysics::Cosmology and Extragalactic Astrophysics, interacting binaries, x-ray, novae, cataclysmic variables, Astrophysics::Solar and Stellar Astrophysics, white-dwarf, accretion, accretion discs, radial-velocity, methods: observational, hubble-space-telescope, stars: individual: ux ursae majoris, ultraviolet-spectroscopic-explorer, Astrophysics::Galaxy Astrophysics, eclipse maps
Abstract

We present an analysis of time-resolved, medium-resolution optical spectroscopic observations of UX Ursae Majoris (UX UMa) in the blue (3920-5250 A) and red (6100-7200 A) wavelength ranges that were obtained in 1999 April and 2008 March, respectively. The observed characteristics of our spectra indicate that UX UMa has been in different states during those observations. The blue spectra are very complex. They are dominated by strong and broad single-peaked emission lines of hydrogen. The high-excitation lines of He ii lambda 4686 and the Bowen blend are quite strong as well. All the lines consist of a mixture of absorption and emission components. Using Doppler tomography, we have identified four distinct components of the system: the accretion disc, the secondary star, the bright spot from the gas stream/disc impact region and the unique compact area of absorption in the accretion disc seen as a dark spot in the lower left-hand quadrant of the tomograms. In the red wavelength range, both the hydrogen (H alpha) and neutral helium (He i lambda 6678 and He i lambda 7065) lines were observed in emission and both exhibited double-peaked profiles. Doppler tomography of these lines reveals spiral structure in the accretion disc, but in contrast to the blue wavelength range, there is no evidence for either the dark spot or the gas stream/disc impact region emission, while the emission from the secondary star is weak. During the observations in 1999, UX UMa showed many of the defining properties of the SW Sextantis stars. However, all these features almost completely disappeared in 2008. We have also estimated the radial velocity semi-amplitudes K-1 and K-2 and evaluated the system parameters of UX UMa. These estimates are inconsistent with previous values derived by means of analysis of white dwarf eclipse features in the light curve in different wavelength ranges.

Published
2010

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