Correlation of the estimated arrival time of the relativistic solar ions at 1 AU and start of ground level enhancement (GLE)

H. Martirosyan; A. Chilingarian

Home/Archive/arXiv

arXiv · astro-ph/0507414

Correlation of the estimated arrival time of the relativistic solar ions at 1 AU and start of ground level enhancement (GLE)

H. Martirosyan·A. Chilingarian

View original source ↗Read source document ↗Export metadata ↓

Abstract

We are investigated possible correlations between the calculated arrival times of the first relativistic ions at Earth and GLE start times registered by surface monitors. The analysis is based on the arrival times and energies of the first solar ions, registered by the Solar Isotope Spectrometer (SIS) on board of the ACE satellite, and protons, registered by GOES satellites. We consider both cases when the interplanetary propagation of the first high energy ions is essentially scatter-free and the diffusion of high energy ions during propagation in the interplanetary magnetic field. We extrapolate the time-velocity and time-rigidity relationships to calculate the expected arrival times of the relativistic ions that are energetic enough to enter the atmosphere at the Aragats geographical location and produce secondary fluxes that reach the monitors.

Explore related subjects

astro-ph

Keep this discovery

Explore connections, maps & timelines

BibTeX RIS

H. Martirosyan, A. Chilingarian. 2005-07-18. Correlation of the estimated arrival time of the relativistic solar ions at 1 AU and start of ground level enhancement (GLE). https://arxiv.org/abs/astro-ph/0507414

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

arXiv2026

On binary pulsars and the force of gravity

The energy-momentum budget of the astrophysical systems can be studied by the exact local conservation equation derived by Landau and Lifshitz. We show that a similar equation is valid for the Einstein-Cartan gravity. We reanalyze a binary pulsar system using the Landau-Lifshitz conservation equation and show that the orbital period change rate can be completely understood as a curvature backreaction process. Taking into account the detailed theoretical and observational research of relativistic binary pulsar systems, especially the system of Hulse and Taylor, we conclude that general relativity and astrophysical observations rule out the existence of gravitational radiation. We comment upon the LIGO GW events and their alternative explanation, as well as the recent pulsar timing arrays data.

astro-ph↗

arXiv2026

Oscillation frequencies and mode lifetimes in alpha Centauri A

We analyse our recently-published velocity measurements of alpha Cen A (Butler et al. 2004). After adjusting the weights on a night-by-night basis in order to optimize the window function to minimize sidelobes, we extract 42 oscillation frequencies with l=0 to 3 and measure the large and small frequency separations. We give fitted relations to these frequencies that can be compared with theoretical models and conclude that the observed scatter about these fits is due to the finite lifetimes of the oscillation modes. We estimate the mode lifetimes to be 1-2 d, substantially shorter than in the Sun.

astro-ph↗

arXiv2026

Hipparcos period-luminosity relations for Miras and semiregular variables

We present period-luminosity diagrams for nearby Miras and semiregulars, selecting stars with parallaxes better than 20 per cent and well-determined periods. Using K-band magnitudes, we find two well-defined P-L sequences, one corresponding to the standard Mira P-L relation and the second shifted to shorter periods by a factor of about 1.9. The second sequence only contains semiregular variables, while the Mira sequence contains both Miras and semiregulars. Several semiregular stars show double periods in agreement with both relations. The Whitelock evolutionary track is shown to fit the data, indicating that the semiregulars are Mira progenitors. The transition between the two sequences may correspond to a change in pulsation mode or to a change in the stellar structure. Large amplitude pulsations leading to classical Mira classification occur mainly near the tip of the local AGB luminosity function.

astro-ph↗