Observations of Comet Halley 1909 c
نویسندگان
چکیده
منابع مشابه
Polarimetric studies of comet Halley
In the present work, the non-spherical grain characteristics of comet Halley are analysed using the T-matrix method at λ= 0.365,0.485 and 0.684μm respectively. In order to analyse the polarisation data of comet Halley, the dust size distribution function derived by Das et al. (2004) for comet Halley is used in the present work. The size range of the grains is taken to be 0.01μm≤ s ≤ 3μm. Using ...
متن کاملThe Distributed Co in Comet Halley
Examination of the spatial distribution of CO intensity of Comet Halley indicates that a large fraction of CO originates from the refractory organic component in the coma, rather than directly from the volatiles in the nucleus. Based on the fluffy aggregate interstellar dust comet model, we have estimated the upper limits of the total amount of CO provided by coma dust. The implications from th...
متن کاملPickup Protons and Water Ions at Comet Halley Comparisons with Giotto Observations
A quasi-linear diffusion model including both pitch angle and energy diffusion, adiabatic ompression and convective motion with the solar wind flow has been used to investigate the cometary ion pickup process along the Sun-comet line at comet Halley. The total pickup ion densities and magnetic turbulence spectrum levels observed by Giotto were used to constrain the quasi-linear model. Compariso...
متن کاملResonant Behavior of Comet Halley and the Orionid Stream
Comet 1P/Halley has the unique distinction of having a very comprehensive set of observational records for almost every perihelion passage from 240 B.C. This has helped to constrain theoretical models pertaining to its orbital evolution. Many previous works have shown the active role of mean motion resonances in the evolution of various meteoroid streams. Here we look at how various resonances,...
متن کاملCharge-Coupled Device Photometry of Comet P/Halley
Comet P/Halley has been observed during its approach to perihelion at heliocentric distances R = I 1.0 AU and R = 8.2 AU. No extended coma is seen and limits can be placed on the fraction of the total light contributed by coma. The brightness of the comet varies on a short time scale. The variations may be due to transient activity or to rotation of the irregular nucleus. ,. 1984 Academic Pre',...
متن کاملذخیره در منابع من
با ذخیره ی این منبع در منابع من، دسترسی به آن را برای استفاده های بعدی آسان تر کنید
ژورنال
عنوان ژورنال: Astronomische Nachrichten
سال: 1911
ISSN: 0004-6337,1521-3994
DOI: 10.1002/asna.19111871802