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109 results on '"Fu, J.-N."'

101. The pulsation modes of the pre-white dwarf PG 1159-035*

Author

Costa, J. E. S., Kepler, S. O., Winget, D. E., O'Brien, M. S., Kawaler, S. D., Costa, A. F. M., Giovannini, O., Kanaan, A., Mukadam, A. S., Mullally, F., Nitta, A., Provençal, J. L., Shipman, H., Wood, M. A., Ahrens, T. J., Grauer, A., Kilic, M., Bradley, P. A., Sekiguchi, K., Crowe, R., Jiang, X. J., Sullivan, D., Sullivan, T., Rosen, R., Clemens, J. C., Janulis, R., O'Donoghue, D., Ogloza, W., Baran, A., Silvotti, R., Marinoni, S., Vauclair, G., Dolez, N., Chevreton, M., Dreizler, S., Schuh, S., Deetjen, J., Nagel, T., Solheim, J.-E., Gonzalez Perez, J. M., Ulla, A., Barstow, M., Burleigh, M., Good, S., Metcalfe, T. S., Kim, S.-L., Lee, H., Sergeev, A., Akan, M. C., Çakırlı, Ö., Paparo, M., Viraghalmy, G., Ashoka, B. N., Handler, G., Hürkal, Ö., Johannessen, F., Kleinman, S. J., Kalytis, R., Krzesinski, J., Klumpe, E., Larrison, J., Lawrence, T., Meištas, E., Martinez, P., Nather, R. E., Fu, J.-N., Pakštienė, E., Rosen, R., Romero-Colmenero, E., Riddle, R., Seetha, S., Silvestri, N. M., Vučković, M., Warner, B., Zola, S., Althaus, L. G., Córsico, A. H., Montgomery, M. H., Costa, J. E. S., Kepler, S. O., Winget, D. E., O'Brien, M. S., Kawaler, S. D., Costa, A. F. M., Giovannini, O., Kanaan, A., Mukadam, A. S., Mullally, F., Nitta, A., Provençal, J. L., Shipman, H., Wood, M. A., Ahrens, T. J., Grauer, A., Kilic, M., Bradley, P. A., Sekiguchi, K., Crowe, R., Jiang, X. J., Sullivan, D., Sullivan, T., Rosen, R., Clemens, J. C., Janulis, R., O'Donoghue, D., Ogloza, W., Baran, A., Silvotti, R., Marinoni, S., Vauclair, G., Dolez, N., Chevreton, M., Dreizler, S., Schuh, S., Deetjen, J., Nagel, T., Solheim, J.-E., Gonzalez Perez, J. M., Ulla, A., Barstow, M., Burleigh, M., Good, S., Metcalfe, T. S., Kim, S.-L., Lee, H., Sergeev, A., Akan, M. C., Çakırlı, Ö., Paparo, M., Viraghalmy, G., Ashoka, B. N., Handler, G., Hürkal, Ö., Johannessen, F., Kleinman, S. J., Kalytis, R., Krzesinski, J., Klumpe, E., Larrison, J., Lawrence, T., Meištas, E., Martinez, P., Nather, R. E., Fu, J.-N., Pakštienė, E., Rosen, R., Romero-Colmenero, E., Riddle, R., Seetha, S., Silvestri, N. M., Vučković, M., Warner, B., Zola, S., Althaus, L. G., Córsico, A. H., and Montgomery, M. H.

Abstract

Context.PG 1159-035, a pre-white dwarf with $T_{{\rm eff}}$$\simeq$140 000 K, is the prototype of both two classes: the PG 1159 spectroscopic class and the DOV pulsating class. Previous studies of PG 1159-035photometric data obtained with the Whole Earth Telescope (WET) showed a rich frequency spectrum allowing the identification of 122 pulsation modes. Analyzing the periods of pulsation, it is possible to measure the stellar mass, the rotational period and the inclination of the rotation axis, to estimate an upper limit for the magnetic field, and even to obtain information about the inner stratification of the star.

Published
2008
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102. Frequency Oscillations in the Delta Scuti Star V534 Tauri: Preliminary Results of the STEPHI IX Campaign

Author

Machado, L. Fox, primary, Li, Z. P., additional, Michel, E., additional, Alvarez, M., additional, Hernández, M. M., additional, Chevreton, M., additional, Zhou, A., additional, Barban, C., additional, Dolez, N., additional, Belmonte, J. A., additional, Fernández, A., additional, Fremy, J., additional, Pau, S., additional, Servan, B., additional, Hernández, F. Pérez, additional, Liu, Y. Y., additional, Fu, J. N., additional, and Ringot, O., additional

Published
2000
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104. Pulsation of the δScuti star VZ Cancri

Author

Fu, J.-N., Jiang, S.-Y., Fu, J.-N., and Jiang, S.-Y.

Abstract

After the "$\rm O-C$” technique is used to study the pulsation of the δScuti star VZ Cnc with the times of maximum light listed in the literature and a newly-determined time based on new photometry for this star, some high-quality photometry light curves in the literature are analysed by the Fourier decomposition, showing that there are more than 2 frequencies in the pulsation of this star, which might be one possible explanation of the existence of the large scatter in the "$\rm O-C$” diagram.

Published
1999
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105. Asteroseismology of the ZZ Ceti star HS 0507+0434B★.

Author

Fu, J.-N., Dolez, N., Vauclair, G., Machado, L. Fox, Kim, S.-L., Li, C., Chen, L., Alvarez, M., Su, J., Charpinet, S., Chevreton, M., Michel, R., Yang, X. H., Li, Y., Zhang, Y. P., Molnar, L., and Plachy, E.

Subjects
WHITE dwarf stars, STELLAR oscillations, CONSTRAINTS (Physics), ASTRONOMICAL observations, STELLAR luminosity function, STELLAR rotation, TIME series analysis
Abstract

The pulsating DA white dwarfs (ZZ Ceti stars) are g-mode non-radial pulsators. Asteroseismology provides strong constraints on their global parameters and internal structure. Since all the DA white dwarfs falling in the ZZ Ceti instability strip do pulsate, the internal structure derived from asteroseismology brings knowledge for the DA white dwarfs as a whole group. HS 0507+0434B is one of the ZZ Ceti stars which lies approximately in the middle of the instability strip for which we have undertaken a detailed asteroseismological study. We carried out multisite observation campaigns in 2007 and from 2009 December to 2010 January. In total, 206 h of photometric time series have been collected. They have been analysed by means of Fourier analysis and simultaneous multifrequency sine wave fitting. In total, 39 frequency values are resolved including six triplets and a number of linear combinations. We identify the triplets as ℓ = 1 g modes split by rotation. We derived the period spacing, the rotational splitting and the rotation rate. From the comparison of the observed periods with the theoretical periods of a series of models, we estimate the fundamental parameters of the star: its total mass M*/M⊙ = 0.675, its luminosity L/L⊙ = 3.5 × 10−3, and its hydrogen mass fraction MH/M* = 10−8.5. [ABSTRACT FROM AUTHOR]

Published
2013
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106. Pulsations and Period Changes of the SX Phoenicis Star DY PegasiBased on data obtained at Xinglong Station of the National Astronomical Observatories, and Lijiang Station of Yunnan Astronomical Observatory, Chinese Academy of Sciences, China.

Author

Fu, J. N., Zha, Q., Zhang, Y. P., Chen, L., Poon, H., Marak, K., Boonyarak, C., Khokhuntod, P., Su, J., Li, Y., Zhang, C., and Jiang, S. Y.

Abstract

We present 83 new times of maximum light of the SX Phoenicis (SX Phe) star DY Pegasi (DY Peg), based mainly on our new time-series photometric observations from the years 2004-2008. Together with the times of maximum light in the literature, a comprehensive study of the O- Cdiagram with the data spanning over seven decades leads to a new general ephemeris formula and the determination of a new value of the updated period 0.072926187( ± 3)d. The available times of maximum light can be well modeled with either a triple linear fit, or a fit concerning a continuously increasing period change combined with the light-time effect of an orbital motion. On the contrary, the decreasing period hypothesis suggested by some previous investigators appears to be rejected. The frequency analyses of the data collected in 2004 and 2006 provide the radial pulsation frequency 13.713 cd-1and its four harmonics. However, although extra powers were present around the reported secondary frequency 17.8 cd-1in the Fourier transformations of the new data sets, its signal-to-noise ratios were too low to detect this frequency.

Published
2009
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108. VizieR Online Data Catalog: LAMOST DR1 catalogs (Luo+, 2015)

Author

Luo, A. -L, Zhao, Y. -H, Zhao, G., Deng, L. -C, Liu, X. -W, Jing, Y. -P, Wang, G., Zhang, H. -T, Shi, J. -R, Cui, X. -Q, Chu, Y. -Q, Li, G. -P, Bai, Z. -R, Wu, Y., Cai, Y., Cao, S. -Y, Cao, Z. -H, Jeffrey Carlin, Chen, H. -Y, Chen, J. -J, Chen, K. -X, Chen, L., Chen, X. -L, Chen, X. -Y, Chen, Y., Christlieb, N., Chu, J. -R, Cui, C. -Z, Dong, Y. -Q, Du, B., Fan, D. -W, Feng, L., Fu, J. -N, Gao, P., Gong, X. -F, Gu, B. -Z, Guo, Y. -X, Han, Z. -W, He, B. -L, Hou, J. -L, Hou, Y. -H, Hou, W., Hu, H. -Z, Hu, N. -S, Hu, Z. -W, Huo, Z. -Y, Jia, L., Jiang, F. -H, Jiang, X., Jiang, Z. -B, Jin, G., Kong, X., Lei, Y. -J, Li, A. -H, Li, C. -H, Li, G. -W, Li, H. -N, Li, J., Li, Q., Li, S., Li, S. -S, Li, X. -N, Li, Y., Li, Y. -B, Li, Y. -P, Liang, Y., Lin, C. -C, Liu, C., Liu, G. -R, Liu, G. -Q, Liu, Z. -G, Lu, W. -Z, Luo, Y., Mao, Y. -D, Newberg, H., Ni, J. -J, Qi, Z. -X, Qi, Y. -J, Shen, S. -Y, Shi, H. -M, Song, J., Song, Y. -H, Su, D. -Q, Su, H. -J, Tang, Z. -H, Tao, Q. -S, Tian, Y., Wang, D., Wang, D. -Q, Wang, F. -F, Wang, G. -M, Wang, H., Wang, H. -C, Wang, J., Wang, J. -N, Wang, J. -L, Wang, J. -P, Wang, J. -X, Wang, L., Wang, M. -X, Wang, S. -G, Wang, S. -Q, Wang, X., Wang, Y. -N, Wang, Y., Wang, Y. -F, Wei, P., Wei, M. -Z, Wu, H., Wu, K. -F, Wu, X. -B, Wu, Y. -Z, Xing, X. -Z, Xu, L. -Z, Xu, X. -Q, Xu, Y., Yan, T. -S, Yang, D. -H, Yang, H. -F, Yang, H. -Q, Yang, M., Yao, Z. -Q, Yu, Y., Yuan, H., Yuan, H. -B, Yuan, H. -L, Yuan, W. -M, Zhai, C., Zhang, E. -P, Zhang, H. -W, Zhang, J. -N, Zhang, L. -P, Zhang, W., Zhang, Y., Zhang, Y. -X, Zhang, Z. -C, Zhao, M., Zhou, F., Zhou, X., Zhu, J., Zhu, Y. -T, Zou, S. -C, and Zuo, F.

109. LONG AND CONSECUTIVE OBSERVATIONS OF FOUR ECLIPSING BINARY STARS FROM DOME A, ANTARCTICA.

Author

Huang, Z. H., Fu, J. N., and Zong, W. K.

Subjects
*STAR observations, *ECLIPSING binaries, *BINARY systems (Astronomy), *PARAMETER estimation, *STELLAR mass
Abstract

Dome A, on the Antarctica plateau, offers a new window for uninterrupted and consecutive observations of variable targets. CSTAR deployed at Dome A had been operated for four consecutive years since 2008 and collected vast mass of frames. For each polar winter, the observational time can span over 100 days which means to cover hundreds of periods of most eclipsing binary stars. We represent here the first result of four eclipsing binary stars, CSTAR 36162, CSTAR 38663, CSTAR 55495 and CSTAR 57775, using the data of CSTAR 2008 in i and 2009 in g and r bands. The further works are in progress, including fundamental parameters of those targets using the WD's code and investigation of period change from O -- C diagrams. [ABSTRACT FROM AUTHOR]

Published
2013
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