Three cases of large-amplitude, small spatial-scale interplanetary particle gradients observed by the anticoincidence shield (ACS) aboard the INTEGRAL spacecraft in 2006 are investigated. The high data rates provided by the INTEGRAL ACS allow an unprecedented ability to probe the fine structure of GCR propagation in the inner Heliosphere. For two of the three cases, calculating perpendicular and parallel cosmic ray diffusion coefficients based on both field and particle data results in parallel diffusion appearing to satisfy a convection gradient current balance, provided that the magnetic scattering of the particles can be described by quasi-linear theory. In the third case, perpendicular diffusion seems to dominate. The likelihood of magnetic flux rope topologies within solar ejecta affecting the local modulation is considered, and its importance in understanding the field-particle interaction for the astrophysics of nonthermal particle phenomena is discussed.

John J. Quenby

Tamitha Mulligan

J. Bernard Blake

Diana N. A. Shaul

Diffusion Coefficients, Short-Term Cosmic Ray Modulation, and Convected Magnetic Structures

The anomalous microwave emission (AME) has been proved to be an important component of the galactic
diffuse emission in the range from 20 to 60&#x2009;GHz. To discriminate between different models of AME, low frequency microwave data from 10 to 20&#x2009;GHz are needed. We present here a reanalysis of published and unpublished Tenerife data from 10 to 33&#x2009;GHz at large angular scales (from 5 to 15 degrees). We cross-correlate the Tenerife data to templates of the main galactic diffuse emissions: synchrotron, free-free, and thermal dust. We find evidence of dust-correlated emission in the Tenerife data that could be explained as spinning dust grain emission.

J. F. Mac&#xed;as-P&#xe9;rez

R. D. Davies

R. Watson

C. M. Gutierrez

R. Rebolo

A Characterization of the Diffuse Galactic Emissions at Large Angular Scales Using the Tenerife Data

The <i>Planck</i> 28.5&#x2009;GHz maps were searched for potential Anomalous Microwave Emission (AME) regions on the scale of <i>&#x7e;</i>3&#xb0; or smaller, and several new regions of interest were selected. Ancillary data at both lower and higher frequencies were used to construct spectral energy distributions (SEDs), which seem to confirm an excess consistent with spinning dust models. Here we present higher resolution observations of two of these new regions with the Arcminute Microkelvin Imager Small Array (AMI SA) between 14 and 18&#x2009;GHz to test for the presence of a compact (<i>&#x7e;</i>10 arcmin or smaller) component. For AME-G107.1+5.2, dominated by the Hii region S140, we find evidence for the characteristic rising spectrum associated with either the spinning dust mechanism for AME or an ultra- /hypercompact Hii region across the AMI frequency band; however, for AME-G173.6+208 we find no evidence for AME on scales of <i>&#x7e;</i>2&#x2013;10 arcmin.

Yvette C. Perrott

Anna M. M. Scaife

Natasha Hurley-Walker

Keith J. B. Grainge

Investigating the Source of Planck-Detected AME: High-Resolution Observations at 15&#x2009;GHz

We present a new redshift (RS) versus photon travel time (<svg     style="vertical-align:-3.43848pt;width:12.25px;" id="M1" height="14.475" version="1.1" viewBox="0 0 12.25 14.475" width="12.25"  xmlns:xlink="http://www.w3.org/1999/xlink" xmlns="http://www.w3.org/2000/svg">
	
		
			<g transform="matrix(.017,-0,0,-.017,.062,10.125)"><path id="x1D461" d="M324 430l-26 -36l-112 -4l-55 -265q-13 -66 7 -66q13 0 44.5 20t50.5 40l17 -24q-38 -40 -85.5 -73.5t-87.5 -33.5q-50 0 -21 138l55 262h-80l-2 8l25 34h66l25 99l78 63l10 -9l-37 -153h128z" /></g>

			<g transform="matrix(.012,-0,0,-.012,5.862,14.2)"><path id="x1D446" d="M457 488l-30 -3q-17 148 -131 148q-53 0 -84.5 -34.5t-31.5 -82.5q0 -42 25.5 -72t74.5 -62l33 -22q63 -42 95 -85t32 -102q0 -84 -67 -137t-163 -53q-58 0 -113 22t-70 43l-4 152l27 4q4 -32 15 -62.5t31 -59.5t53.5 -47t76.5 -18q56 0 92 35t36 96q0 39 -25 70t-78 68&#xA;l-31 22q-32 23 -53.5 41.5t-45 57t-23.5 77.5q0 82 58 132.5t156 50.5q46 0 101 -17l18.5 -6t17 -6t8.5 -3q-4 -55 0 -147z" /></g>

		
	
</svg>) test including 171 supernovae RS data points. We extended the Hubble diagram to a range of <i  >z</i> = 0,0141&#x2013;8.1 in the hope that at high RSs, the fitting of the calculated RS/<svg     style="vertical-align:-3.43848pt;width:12.25px;" id="M2" height="14.475" version="1.1" viewBox="0 0 12.25 14.475" width="12.25"  xmlns:xlink="http://www.w3.org/1999/xlink" xmlns="http://www.w3.org/2000/svg">
	
		
			<g transform="matrix(.017,-0,0,-.017,.062,10.125)"><use xlink:href="#x1D461"/></g>

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</svg> diagrams to the observed RS data would, as predicted by different cosmological models, set constraints on alternative cosmological models. The Lambda cold dark matter (&#x39b;CDM), the static universe model, and the case for a slowly expanding flat universe (SEU) are considered. We show that on the basis of the Hubble diagram test, the static and the slowly expanding models are favored.

Laszlo A. Marosi

Hubble Diagram Test of Expanding and Static Cosmological Models: The Case for a Slowly Expanding Flat Universe

We analyzed the high-energy gamma and neutron emissions observed by the SONG instrument onboard the CORONAS-F satellite during August 25, 2001, October 28, 2003, November 4, 2003, and January 20, 2005 solar flares. These flares produced neutrons and/or protons recorded near Earth. The SONG response was consistent with detection of the pion-decay gamma emission and neutrons in these events. We supposed that a time profile of the soft X-ray derivative was a good proxy of time behavior of the flare energy release. Then we showed that time intervals of the maximum both of energy release and pion-decay-emission coincided well. We determined the onset time of GLEs 65, 69 on the basis of neutron monitor data using the superposed epoch method. The time of high-energy proton onset on November 4, 2003 was found from the GOES data. The time delay between the high-energy gamma ray observation and the high-energy protons onset time was &#x3c;5 minutes. This time lag corresponds to the least possible proton propagation time. So, we conclude that in these events both protons interacted in the solar atmosphere and the first protons which arrived to Earth, belonged to one and the same population of the accelerated particles.

Viktoria Kurt

Karel Kudela

Boris Yushkov

Vladimir Galkin

On the Onset Time of Several SPE/GLE Events: Indications from High-Energy Gamma-Ray and Neutron Measurements by CORONAS-F

Selected activities aimed to investigate cosmic ray fluxes and to contribute to the understanding of the mechanisms behind, over a long-time period using space research tools in the former USSR/Russia and Slovakia, are reviewed, and some of the results obtained are presented. As the selection is connected with the institutes where the authors are working, it represents only a partial review of this wide topic.

Yu. I. Logachev

L. L. Lazutin

K. Kudela

Cosmic Ray Investigation in the Stratosphere and Space: Results from Instruments on Russian Satellites and Balloons

I give a summary of the observations of Anomalous Microwave Emission (AME) from HII regions. AME has been detected in, or in the vicinity of, HII regions. Given the difficulties in measuring accurate SEDs over a wide range of frequencies and in complex environments, many of these detections require more data to confirm them as emitting significant AME. The contribution from optically thick
free-free emission from UCHII regions may be also be significant in some cases. The AME emissivity, defined as the ratio of the AME brightness to the 100&#x2009;<i>&#x3bc;</i>m brightness, is comparable to the value observed in high-latitude diffuse cirrus in some regions, but is significantly lower in others. However, this value is dependent on the dust temperature. More data, both at high frequencies (&#x3e;<i>&#x7e;</i>5&#x2009;GHz) and high resolution (<i>&#x7e;</i>1&#x2032; or better) is required to disentangle the emission processes in such complex regions.

Clive Dickinson

Observations of Anomalous Microwave Emission from HII Regions

Using the Archeops and WMAP data, we perform a study of the anticenter Galactic diffuse emissions&#x2014;thermal dust, synchrotron, free-free, and anomalous emissions&#x2014;at degree scales. The high-frequency data are used to infer the thermal dust electromagnetic spectrum and spatial distribution allowing us to precisely subtract this component at lower frequencies. After subtraction of the thermal dust component, a mixture of standard synchrotron and free-free emissions does not account for the residuals at these low frequencies. Including the all-sky 408&#x2009;MHz Haslam data we find evidence for anomalous emission with a spectral index of &#x2212;2.5 in <svg     style="vertical-align:-4.8526pt;width:23.375px;" id="M1" height="17.6625" version="1.1" viewBox="0 0 23.375 17.6625" width="23.375"  xmlns:xlink="http://www.w3.org/1999/xlink" xmlns="http://www.w3.org/2000/svg">
	
		
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			<g transform="matrix(.012,-0,0,-.012,11.388,15.637)"><path id="x52" d="M631 18l-4 -26q-24 0 -35 1q-57 3 -92.5 23t-69.5 68q-21 30 -101 160q-13 22 -30.5 31t-54.5 9h-32v-159q0 -63 14 -77.5t74 -19.5v-28h-262v28q62 5 76 19.5t14 77.5v402q0 62 -13 76t-73 19v28h248q109 0 159 -34q67 -42 67 -131q0 -115 -127 -172q27 -52 89 -144&#xA;q49 -71 81 -104q31 -36 72 -47zM212 316h48q73 0 108 29q55 42 55 124q0 76 -42 112t-104 36q-41 0 -54 -10q-11 -7 -11 -44v-247z" /></g><g transform="matrix(.012,-0,0,-.012,18.777,15.637)"><path id="x4A" d="M303 650v-28q-58 -5 -71.5 -19.5t-13.5 -77.5v-373q0 -99 -18.5 -156.5t-67.5 -102.5q-49 -44 -93 -58l-12 29q78 38 96 130q10 60 10 191v340q0 63 -14 77.5t-75 19.5v28h259z" /></g>

		
	
</svg> units. However, we are not able to provide coclusion regarding the nature of this anomalous emission in this region. For this purpose, data between 408&#x2009;MHz and 20&#x2009;GHz covering the same sky region are needed.

L. Fauvet

S. R. Hildebrandt

F.-X. D&#xe9;sert

A Characterization of the Diffuse Galactic Emissions in the Anticenter of the Galaxy

This paper reviews the current status of theoretical modeling of electric dipole radiation from spinning dust grains. The fundamentally simple problem of dust grain rotation appeals to a rich set of concepts of classical and quantum physics, owing to the diversity of processes involved. Rotational excitation and damping rates through various mechanisms are discussed, as well as methods of computing the grain angular momentum distribution function. Assumptions on grain properties are reviewed. The robustness of theoretical predictions now seems mostly limited by the uncertainties regarding the grains themselves, namely, their abundance, dipole moments, and size and shape distribution.

Yacine Ali-Ha&#xef;moud

Spinning Dust Radiation: A Review of the Theory

The cosmic rays differential intensity inside the heliosphere, for energy below 30&#x2009;GeV/nuc, depends on solar activity and interplanetary magnetic field polarity. This variation, termed solar modulation, is described using a 2D (radius and colatitude) Monte Carlo approach for solving the Parker transport equation that includes diffusion, convection, magnetic drift, and adiabatic energy loss. Since the whole transport is strongly related to the interplanetary magnetic field (IMF) structure, a better understanding of his description is needed in order to reproduce the cosmic rays intensity at the Earth, as well as outside the ecliptic plane. In this work an interplanetary magnetic field model including the standard description on ecliptic region and a polar correction is presented. This treatment of the IMF, implemented in the HelMod Monte Carlo code (version 2.0), was used to determine the effects on the differential intensity of Proton at 1 AU and allowed one to investigate how latitudinal gradients of proton intensities, observed in the inner heliosphere with the Ulysses spacecraft during 1995, can be affected by the modification of the IMF in the polar regions.

P. Bobik

G. Boella

M. J. Boschini

C. Consolandi

S. Della Torre

M. Gervasi

D. Grandi

S. Pensotti

P. G. Rancoita

D. Rozza

M. Tacconi

Latitudinal Dependence of Cosmic Rays Modulation at 1 AU  and Interplanetary Magnetic Field Polar Correction

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<p><em>Advances in Astronomy</em> publishes in all areas of astronomy, astrophysics, and cosmology, and accepts observational and theoretical investigations into celestial objects and the wider universe.</p>


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<p>Chief Editor, Professor Trigo-Rodríguez (ICE, IEEC-CSIC), has a background in the formation of primitive solar system minor bodies, the study of their fragments in space and the analysis of their surviving rocks that arrived on the Earth.</p>


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Advances in Astronomy - Table of contents 2013

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Advances in Astronomy publishes in all areas of astronomy, astrophysics, and cosmology, and accepts observational and theoretical investigations into celestial objects and the wider universe.

Advances in Astronomy