Hα-Line
Anisotropy in Broad Component of Hα Line in the Magnetospheric Device RT-1
... of Hα line by Doppler spectroscopy. Broad component of Hα line has been ob- served in astrophysical and laboratory ...α line shape by separating charge exchange contribution from other ...
5
The dynamics of rapid redshifted and blueshifted excursions in the solar Hα line
... The observations presented here show that RREs and RBEs either display apparent motions that are directed outwardly from the magnetic bright point, or emerge suddenly within a few seconds. Our very high cadence ( 1.3 s ) ...
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Boötes HiZELS:an optical to near infrared survey of emission line galaxies at z=0 4 4 7
... as Hα 1 , Hβ/[O iii ] 2 and [O ii ], complemented by three blue filters at λ ≈ 390 − 510 nm that select Lyα ...their Hα line at z = ...of line-emitters, their global properties such as number ...
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Small-scale Structuring of Ellerman Bombs at the Solar Limb
... Co-spatial EUV data inferred by the SDO/AIA in- strument are also analysed for each EB. As EBs con- sist of a vertical extension, one may expect that some signature would be observed in the upper atmo- sphere, however, ...
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Orbital periods of cataclysmic variables identified by the SDSS V, VLT, NTT and Magellan observations of nine equatorial systems
... SDSS J0043 was found to be a CV by Szkody et al. (2004) from an SDSS spectrum which shows a blue continuum with narrow Balmer emission lines. There are very broad Balmer absorption lines attributable to the white dwarf ...
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SPECTROSCOPY OF BRIGHT ALGOL-TYPE SEMI-DETACHED CLOSE BINARY SYSTEM HU TAURI (HR 1471)
... January is well exposed and it is widened to 800 microns and the exposure time was 89 minutes. The violet-shifted emission feature extends very much in to the violet wing of the Hα line. This emission ...
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COMMISSIONS 27 AND 42 OF THE IAU INFORMATION BULLETIN ON VARIABLE STARS
... of Hα line vary slightly from date to ...the Hα profile. Average positions of Hα components correspond to values: V r (blue) = − 180 ...
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Cataclysmic variables from a ROSAT/2MASS selection I, Four new intermediate polars
... Scargle periodogram computed from the radial velocity variation of the Hα line wings in RX J1803, determining the orbital period to be Porb = 160.21 min... The time-resolved spectroscopy[r] ...
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A CANDELS-3D-HST synergy: Resolved Star Formation Patterns at 0.7 < z > 1.5
... of Hα and star formation profiles as a function of galaxy mass and SFR by ...the Hα line emission originates is required for the EW to be an unbiased proxy of the star formation ...intrinsic ...
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A study of accretion and disk diagnostics in the NGC 2264 cluster
... 2013 to characterize the transition disk candidates in terms of various accretion diagnostics Hα line emission, ultraviolet excess, disk parameters IR excess, and stellar parameters mass[r] ...
29
Unresolved fine scale structure in solar coronal loop tops
... the Hα line core from such imaging spectropolarimeters provides an excellent tracer of the magnetic environment of the lower solar atmosphere (Leenaarts et ...in Hα as a proxy for revealing the ...
10
A first catalogue of automatically selected ultraviolet excess sources from the UVEX survey
... Symbiotic stars (see e.g. Corradi et al., 2008 and 2010) are interacting binaries composed of a hot white dwarf, accret- ing from a cool giant companion through a wind or through Roche lobe overflow. Two types “Stellar” ...
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Bombs and flares at the surface and lower atmosphere of the Sun
... Synthetic H α spectra were calculated in 3D non-LTE using the Multi3d code ( Leenaarts & Carlsson 2009 ) . We used a fi ve- level plus continuum hydrogen model atom and modeled the Ly α and Ly β lines using complete ...
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PRECESSION OF THE DISK IN PLEIONE STUDY OF THE H LINE PROFILE
... Katahira et al. (1996) analysed shell RV’s from the two consecutive shell phases separated by some 34 years, and concluded that 28 Tau is a spectroscopic binary with an orbital period of 218 days. The forming of a new ...
8
PERIODIC HEMISSION IN THE ECLIPSING BINARY VV CEPHEI
... At present, just past the time of mid-eclipse, it seems prudent to publish the observa- tional material in hand, and wait for the completion of totality and egress from eclipse. It is hoped that having the complete times ...
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Radiative transfer calculations of the diffuse ionized gas in disc galaxies with cosmic ray feedback
... in line with observed scale ...forbidden line intensities. We show that, to reproduce these line emissions, we require a heating mechanism that affects gas over a larger density range than is ...
14
Na I and Hα absorption features in the atmosphere of MASCARA-2b/KELT-20b
... and Hα (9790 ± 1770 K) lines, ...and Hα lines core, respectively, and to ∼ 4000 K when a totally dissociated hydrogen atmosphere (µ = 1) is ...and Hα lines, re- spectively, obtained assuming µ = 1 ...
14
OMEGA–OSIRIS mapping of emission line galaxies in A901/2:IV Extinction of star formation estimators with inclination
... the Hα and [N II ] emission lines were obtained by the OSIRIS Mapping of Emission-line Galaxies in A901/2 survey (OMEGA, Chies-Santos et ...emission- line spectra were constructed with up to 48 ...
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A 1 4 deg2 blind survey for C II], C III] and C IV at z ∼ 0 7–1 5:II Luminosity functions and cosmic average line ratios
... are indeed not uncommon occurrences at z ∼ 0.7 − 1.5, they are much rarer than Lyα or Hα emitters for a fixed flux limit. C III ] and C IV lines might prove to be a suitable avenue for spectroscopic confirmation ...
11
3D whole prominence fine structure modeling
... assume that the magnetic field does not change considerably on the scale of the cross-section width and thus we use a uni- form dipped magnetic field within an individual prominence plasma fine structure. For simplicity ...
13