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• W3104650140 endingPage "29" @default.
• W3104650140 startingPage "29" @default.
• W3104650140 abstract "We present thirteen epochs of near-infrared (0.8-5 micron) spectroscopic observations of the pre-transitional, gapped disk system in SAO 206462 (=HD 135344B). In all, six gas emission lines (including Br gamma, Pa beta, and the 0.8446 micron line of O I) along with continuum measurements made near the standard J, H, K, and L photometric bands were measured. A mass accretion rate of approximately 2 x 10^-8 solar masses per year was derived from the Br gamma and Pa beta lines. However, the fluxes of these lines varied by a factor of over two during the course of a few months. The continuum also varied, but by only ~30%, and even decreased at a time when the gas emission was increasing. The H I line at 1.083 microns was also found to vary in a manner inconsistent with that of either the hydrogen lines or the dust. Both the gas and dust variabilities indicate significant changes in the region of the inner gas and the inner dust belt that may be common to many young disk systems. If planets are responsible for defining the inner edge of the gap, they could interact with the material on time scales commensurate with what is observed for the variations in the dust, while other disk instabilities (thermal, magnetorotational) would operate there on longer time scales than we observe for the inner dust belt. For SAO 206462, the orbital period would likely be 1-3 years. If the changes are being induced in the disk material closer to the star than the gap, a variety of mechanisms (disk instabilities, interactions via planets) might be responsible for the changes seen. The He I feature is most likely due to a wind whose orientation changes with respect to the observer on time scales of a day or less. To further constrain the origin of the gas and dust emission will require multiple spectroscopic and interferometric observations on both shorter and longer time scales that have been sampled so far." @default.
• W3104650140 created "2020-11-23" @default.
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• W3104650140 date "2011-12-28" @default.
• W3104650140 modified "2023-09-23" @default.
• W3104650140 title "VARIABILITY OF DISK EMISSION IN PRE-MAIN SEQUENCE AND RELATED STARS. II. VARIABILITY IN THE GAS AND DUST EMISSION OF THE HERBIG Fe STAR SAO 206462" @default.
• W3104650140 cites W1617577911 @default.
• W3104650140 cites W1739387363 @default.
• W3104650140 cites W1829490738 @default.
• W3104650140 cites W1964619610 @default.
• W3104650140 cites W1971863457 @default.
• W3104650140 cites W1974771230 @default.
• W3104650140 cites W1989803327 @default.
• W3104650140 cites W2000446280 @default.
• W3104650140 cites W2012630673 @default.
• W3104650140 cites W2012862685 @default.
• W3104650140 cites W2016140455 @default.
• W3104650140 cites W2019754078 @default.
• W3104650140 cites W2023344645 @default.
• W3104650140 cites W2024502805 @default.
• W3104650140 cites W2024605337 @default.
• W3104650140 cites W2025788510 @default.
• W3104650140 cites W2027490520 @default.
• W3104650140 cites W2033700568 @default.
• W3104650140 cites W2034817948 @default.
• W3104650140 cites W2035522472 @default.
• W3104650140 cites W2036696684 @default.
• W3104650140 cites W2042753720 @default.
• W3104650140 cites W2044045143 @default.
• W3104650140 cites W2045683486 @default.
• W3104650140 cites W2051997064 @default.
• W3104650140 cites W2056932217 @default.
• W3104650140 cites W2060583930 @default.
• W3104650140 cites W2060685406 @default.
• W3104650140 cites W2061820060 @default.
• W3104650140 cites W2063988638 @default.
• W3104650140 cites W2068474102 @default.
• W3104650140 cites W2076029332 @default.
• W3104650140 cites W2080430275 @default.
• W3104650140 cites W2080714766 @default.
• W3104650140 cites W2084214142 @default.
• W3104650140 cites W2090374392 @default.
• W3104650140 cites W2096568039 @default.
• W3104650140 cites W2096570366 @default.
• W3104650140 cites W2096594817 @default.
• W3104650140 cites W2112164310 @default.
• W3104650140 cites W2117821269 @default.
• W3104650140 cites W2142220522 @default.
• W3104650140 cites W2144050542 @default.
• W3104650140 cites W2152505725 @default.
• W3104650140 cites W2162810728 @default.
• W3104650140 cites W2167814357 @default.
• W3104650140 cites W2172089030 @default.
• W3104650140 cites W3098075567 @default.
• W3104650140 cites W3098463753 @default.
• W3104650140 cites W3099069130 @default.
• W3104650140 cites W3100829578 @default.
• W3104650140 cites W3101479509 @default.
• W3104650140 cites W3101492032 @default.
• W3104650140 cites W3102204902 @default.
• W3104650140 cites W3102232776 @default.
• W3104650140 cites W3103722753 @default.
• W3104650140 cites W3103993705 @default.
• W3104650140 cites W3104730727 @default.
• W3104650140 cites W3105308410 @default.
• W3104650140 cites W3106480174 @default.
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• W3104650140 doi "https://doi.org/10.1088/0004-637x/745/1/29" @default.
• W3104650140 hasPublicationYear "2011" @default.
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