42,209 research outputs found
Connecting speeds, directions and arrival times of 22 coronal mass ejections from the Sun to 1 AU
Forecasting the in situ properties of coronal mass ejections (CMEs) from
remote images is expected to strongly enhance predictions of space weather, and
is of general interest for studying the interaction of CMEs with planetary
environments. We study the feasibility of using a single heliospheric imager
(HI) instrument, imaging the solar wind density from the Sun to 1 AU, for
connecting remote images to in situ observations of CMEs. We compare the
predictions of speed and arrival time for 22 CMEs (in 2008-2012) to the
corresponding interplanetary coronal mass ejection (ICME) parameters at in situ
observatories (STEREO PLASTIC/IMPACT, Wind SWE/MFI). The list consists of
front- and backsided, slow and fast CMEs (up to ). We
track the CMEs to degrees elongation from the Sun with J-maps
constructed using the SATPLOT tool, resulting in prediction lead times of
hours. The geometrical models we use assume different CME
front shapes (Fixed-, Harmonic Mean, Self-Similar Expansion), and
constant CME speed and direction. We find no significant superiority in the
predictive capability of any of the three methods. The absolute difference
between predicted and observed ICME arrival times is hours (
value of 10.9h). Speeds are consistent to within .
Empirical corrections to the predictions enhance their performance for the
arrival times to hours ( value of 7.9h), and for the speeds
to . These results are important for Solar Orbiter
and a space weather mission positioned away from the Sun-Earth line.Comment: 19 pages, 13 figures, accepted for publication in the Astrophysical
Journa
Wind Power Forecasting Methods Based on Deep Learning: A Survey
Accurate wind power forecasting in wind farm can effectively reduce the enormous impact on grid operation safety when high permeability intermittent power supply is connected to the power grid. Aiming to provide reference strategies for relevant researchers as well as practical applications, this paper attempts to provide the literature investigation and methods analysis of deep learning, enforcement learning and transfer learning in wind speed and wind power forecasting modeling. Usually, wind speed and wind power forecasting around a wind farm requires the calculation of the next moment of the definite state, which is usually achieved based on the state of the atmosphere that encompasses nearby atmospheric pressure, temperature, roughness, and obstacles. As an effective method of high-dimensional feature extraction, deep neural network can theoretically deal with arbitrary nonlinear transformation through proper structural design, such as adding noise to outputs, evolutionary learning used to optimize hidden layer weights, optimize the objective function so as to save information that can improve the output accuracy while filter out the irrelevant or less affected information for forecasting. The establishment of high-precision wind speed and wind power forecasting models is always a challenge due to the randomness, instantaneity and seasonal characteristics
Eruptive Event Generator Based on the Gibson-Low Magnetic Configuration
Coronal Mass Ejections (CMEs), a kind of energetic solar eruptions, are an
integral subject of space weather research. Numerical magnetohydrodynamic (MHD)
modeling, which requires powerful computational resources, is one of the
primary means of studying the phenomenon. With increasing accessibility of such
resources, grows the demand for user-friendly tools that would facilitate the
process of simulating CMEs for scientific and operational purposes. The
Eruptive Event Generator based on Gibson-Low flux rope (EEGGL), a new publicly
available computational model presented in this paper, is an effort to meet
this demand. EEGGL allows one to compute the parameters of a model flux rope
driving a CME via an intuitive graphical user interface (GUI). We provide a
brief overview of the physical principles behind EEGGL and its functionality.
Ways towards future improvements of the tool are outlined
Modeling the Young Sun's Solar Wind and its Interaction with Earth's Paleomagnetosphere
We present a focused parameter study of solar wind - magnetosphere
interaction for the young Sun and Earth, Ga ago, that relies on
magnetohydrodynamic (MHD) simulations for both the solar wind and the
magnetosphere. By simulating the quiescent young Sun and its wind we are able
to propagate the MHD simulations up to Earth's magnetosphere and obtain a
physically realistic solar forcing of it. We assess how sensitive the young
solar wind is to changes in the coronal base density, sunspot placement and
magnetic field strength, dipole magnetic field strength and the Sun's rotation
period. From this analysis we obtain a range of plausible solar wind conditions
the paleomagnetosphere may have been subject to. Scaling relationships from the
literature suggest that a young Sun would have had a mass flux different from
the present Sun. We evaluate how the mass flux changes with the aforementioned
factors and determine the importance of this and several other key solar and
magnetospheric variables with respect to their impact on the
paleomagnetosphere. We vary the solar wind speed, density, interplanetary
magnetic field strength and orientation as well as Earth's dipole magnetic
field strength and tilt in a number of steady-state scenarios that are
representative of young Sun-Earth interaction. This study is done as a first
step of a more comprehensive effort towards understanding the implications of
Sun-Earth interaction for planetary atmospheric evolution.Comment: 16 pages, 7 figure
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