D
D. R. McMullin
Researcher at Praxis
Publications - 8
Citations - 1940
D. R. McMullin is an academic researcher from Praxis. The author has contributed to research in topics: Coronal loop & Irradiance. The author has an hindex of 5, co-authored 8 publications receiving 1741 citations.
Papers
More filters
Journal ArticleDOI
Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI)
Russell A. Howard,John D. Moses,Angelos Vourlidas,Jeffrey S. Newmark,Dennis G. Socker,Simon Plunkett,Clarence M. Korendyke,J. W. Cook,A. Hurley,Joseph M. Davila,William T. Thompson,O. C. St. Cyr,E. Mentzell,Kimberly I. Mehalick,James R. Lemen,Jean-Pierre Wuelser,Dexter W. Duncan,T. D. Tarbell,C. J. Wolfson,A. Moore,Richard A. Harrison,Nicholas R. Waltham,J. Lang,Christopher J. Davis,C. J. Eyles,H. Mapson-Menard,G. M. Simnett,Jean-Philippe Halain,Jean-Marc Defise,Emmanuel Mazy,Pierre Rochus,Raymond Mercier,Marie-Françoise Ravet,Franck Delmotte,F. Auchère,Jean-Pierre Delaboudiniere,Volker Bothmer,W. Deutsch,Dennis Wang,N. Rich,S. Cooper,V. Stephens,G. Maahs,R. Baugh,D. R. McMullin,T. Carter +45 more
TL;DR: The Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) is a five telescope package, which has been developed for the Solar Terrestrial Relation Observatory (STEREO) mission.
Journal ArticleDOI
Solar EUV and UV spectral irradiances and solar indices
TL;DR: In this article, the authors analyzed the long-term correspondence of four solar activity index time series International Sunspot Number, the He 1083 Equivalent Width, F 10.7, and the Mg II core-to-wing ratio.
Journal ArticleDOI
The Heliospheric HeII 30.4 nm Solar Flux During Cycle 23
TL;DR: In this paper, a technique for computing the He II 30.4 nm flux at an arbitrary position in the heliosphere from Solar and Heliospheric Observatory (SOHO) EUV Imaging Telescope (EIT) images was described.
Journal ArticleDOI
Model of the all-sky He II 30.4 nm solar flux
TL;DR: In this article, an empirical model of the all-sky He II 30.4 nm flux based on EIT/SOHO data was found to be strongly anisotropic, and the anisotropy I pol /I eq between the fluxes computed for viewpoints located above the solar poles and within the solar equatorial plane ranges from 0.9 at solar minimum to 0.6 at solar maximum.