Sidereal Time Research Articles

Remote viewing as applied to futures studies

Remote viewing is set of related protocols that allow a viewer to intuitively gather information regarding a specific target that is hidden from physical view and separated from the viewer by either time or distance. Research suggests that the same processes used to gather spatially non-local information can also be used to gather information that is temporally removed from the observer. This paper reviews the most common protocols for remote viewing — including Coordinate Remote Viewing (CRV), Associative Remote Viewing (ARV), and Extended Remote Viewing (ERV). 1 1 I gratefully acknowledge the guidance of Emeritus Professor Oliver Markley, who served as a mentor for the research leading to this paper. This remains a controversial field of study. While over 30 years of data has been gathered with statistically significant results frequently occurring under laboratory conditions, skeptics are not convinced that RV is a useful pursuit. In addition to this, some of the output from RV can be vague and subject to personal interpretation. A number of factors have been shown to improve the success rate for remote viewing, including the use of experienced subjects, individual testing, feedback of results, and a short time-interval between the percipient response and the targeted future event. Finally, there also appears to be a relationship between the effectiveness of remote viewing efforts and sidereal time, which may be interpreted as evidence that some aspects of RV are subject to the same physical laws as are other phenomena studied by science. Remote viewing and related processes merit further exploration and study. While remote viewing may never be completely understood, it has the potential to make a meaningful contribution to the professional futurist′s toolbox.

Anisotropy and Corotation of Galactic Cosmic Rays

The intensity of Galactic cosmic rays is nearly isotropic because of the influence of magnetic fields in the Milky Way. Here, we present two-dimensional high-precision anisotropy measurement for energies from a few to several hundred teraelectronvolts (TeV), using the large data sample of the Tibet Air Shower Arrays. Besides revealing finer details of the known anisotropies, a new component of Galactic cosmic ray anisotropy in sidereal time is uncovered around the Cygnus region direction. For cosmic-ray energies up to a few hundred TeV, all components of anisotropies fade away, showing a corotation of Galactic cosmic rays with the local Galactic magnetic environment. These results have broad implications for a comprehensive understanding of cosmic rays, supernovae, magnetic fields, and heliospheric and Galactic dynamic environments.

Transient Detection Using Panoramic All-Sky Cameras

A method of using on-going panoramic all-sky monitors for the purpose of bright optical transient detection is described. The detection is performed by comparing all-sky images to canonical images taken at the same sidereal time. The described approach has been implemented and tested using the infrastructure of the Night Sky Live network of panoramic all-sky cameras. Preliminary results of detected bright flashes are presented in the paper.

High precision methods for locating the celestial intermediate pole and origin

Context.The precession-nutation transformation describes the changing directions on the celestial sphere of the Earth's pole and an adopted origin of right ascension. The coordinate system for the celestial sphere is the geocentric celestial reference system, and the two directions are the celestial intermediate pole (CIP) and the celestial intermediate origin (CIO), the latter having supplanted the equinox for this purpose following IAU resolutions in 2000. The celestial coordinate triad based on the CIP and CIO is called the celestial intermediate reference system; the prediction of topocentric directions additionally requires the Earth rotation angle (ERA), the counterpart of Greenwich sidereal time (GST) in the former equinox based system.

Analysis of cosmic ray anisotropy around 10 15 eV using network observation data of air showers

To study the cosmic ray anisotropy, a harmonic analysis is performed on the EAS arrrival LSTs (local sidereal times) observed by the LAAS group. The amplitude and phase of the first harmonic obtained are 0.23 ± 0.04 % and 0.4 ± 0.7 hr LST in the energy region from 5 × 10 13 to 10 15 eV .

Gravitational wave detection by a spherical antenna: The angular sensitivity of resonators in the truncated icosahedral gravitational wave antenna configuration and its variation with sidereal time and galactic longitude

Experimental projects using spherical antennas to detect gravitational waves are nowdays a concrete reality. The main purpose of this paper is to give a possible way of interpreting output data from such a system. Responses of the five fundamental quadrupole modes and of the six resonators in TIGA collocations are shown as a function of the incoming direction of the incident wave. Then, for a source lying in the galactic plane, sidereal time and galactic longitude dependence is given. Thus, once a candidate source of gravitational waves is considered, we can exactly predict the resonators' response as a function of time.

Tests of Lorentz violation inν¯μ→ν¯eoscillations

A recently developed standard-model extension (SME) formalism for neutrino oscillations that includes Lorentz and $CPT$ violation is used to analyze the sidereal time variation of the neutrino event excess measured by the liquid scintillator neutrino detector (LSND) experiment. The LSND experiment, performed at Los Alamos National Laboratory, observed an excess, consistent with neutrino oscillations, of ${\overline{\ensuremath{\nu}}}_{e}$ in a beam of ${\overline{\ensuremath{\nu}}}_{\ensuremath{\mu}}$. It is determined that the LSND oscillation signal is consistent with no sidereal variation. However, there are several combinations of SME coefficients that describe the LSND data; both with and without sidereal variations. The scale of Lorentz and $CPT$ violation extracted from the LSND data is of order ${10}^{\ensuremath{-}19}\text{ }\text{ }\mathrm{GeV}$ for the SME coefficients ${a}_{L}$ and $E\ifmmode\times\else\texttimes\fi{}{c}_{L}$. This solution for Lorentz and $CPT$ violating neutrino oscillations may be tested by other short baseline neutrino oscillation experiments, such as the MiniBooNE experiment.

All‐Sky Relative Opacity Mapping Using Nighttime Panoramic Images

ABSTRACTAn all‐sky cloud‐monitoring system that generates relative opacity maps over many of the world’s premier astronomical observatories is described. Photometric measurements of numerous background stars are combined with simultaneous sky brightness measurements to differentiate thin clouds from sky glow sources such as airglow and zodiacal light. The system takes a continuous pipeline of all‐sky images and compares them to canonical images taken on other nights at the same sidereal time. Data interpolation then yields transmission maps covering almost the entire sky. An implementation of this system is currently operating through the Night Sky Live network of CONCAM3s located at Cerro Pachón (Chile), Mauna Kea (Hawaii), Haleakala (Hawaii), SALT (South Africa), and the Canary Islands (Northwestern Africa).

Large-Scale Sidereal Anisotropy of Galactic Cosmic-Ray Intensity Observed by the Tibet Air Shower Array

We present the large-scale sidereal anisotropy ofgalactic cosmic-ray intensity in the multi-TeV region observed with the Tibet-IIIair shower array during the period from 1999 through 2003. The sidereal daily variation of cosmic rays observed in this experiment shows an excess of relative intensity around $4\sim7 $ hours local sidereal time, as well as a deficit around 12 hours local sidereal time. While the amplitude of the excess is not significant when averaged over all declinations, the excess in individual declinaton bands becomes larger and clearer as the viewing direction moves toward the south. The maximum phase of the excess intensity changes from $\sim$7 at the northern hemisphere to $\sim$4 hours at the equatorial region. We also show that both the amplitude and the phase of the first harmonic vector of the daily variation are remarkably independent of primary energy in the multi-TeV region. This is the first result determining the energy and declination dependences of the full 24-hour profiles of the sidereal daily variation in the multi-TeV region with a single air shower experiment.

Solar compass chip

A solar compass chip (SCC) is a photosensitive chip with MEMS-based optics (pinhole aperture array) integrated on the chip itself. The MEMS-based optics enables the chip to image the sun. Image processing of the sun image is performed externally to the SCC (typically a processor connected to the SCC). The sun is observed for a period of time, say half an hour, and the angles to the sun are calculated. During that period of time, the sun will slew across the sky due to the sidereal rate. A circle on the surface of a sphere can be fitted to the arc on the sky that the sun traverses. The center of this circle is the rotation axis of the Earth. Besides performing the function of a compass, the SCC can be combined with a clock to establish a three-axis inertial-based coordinate system, or if the vertical is known, to determine the geographic position. A number of commercial applications in the automotive, agricultural, and maritime areas are identified.

Considerations on coincidence experiments between two gravitational wave detectors for sources in the Galactic Centre

In a coincidence experiment between gravitational wave detectors, the sidereal time analysis can provide very useful and powerful indications. We studied, with the help of a MonteCarlo simulation, the sidereal time pattern to be expected in such an experiment in the particular case of the resonant bars NAUTILUS and EXPLORER and for sources located in the Galactic Centre. It is shown that for linearly polarized gravitational waves the sidereal time pattern exhibits just a large peak at hour 3.5 and only a small peak at about hour 12.

Expressions for IAU 2000 precession quantities

A new precession-nutation model for the Celestial Intermediate Pole (CIP) was adopted by the IAU in 2000 (Resolution B1.6). The model, designated IAU 2000A, includes a nutation series for a non-rigid Earth and corrections for the precession rates in longitude and obliquity. The model also specifies numerical values for the pole osets at J2000.0 between the mean equatorial frame and the Geocentric Celestial Reference System (GCRS). In this paper, we discuss precession models consistent with IAU 2000A precession-nutation (i.e. MHB 2000, provided by Mathews et al. 2002) and we provide a range of expressions that implement them. The final precession model, designated P03, is a possible replacement for the precession com- ponent of IAU 2000A, oering improved dynamical consistency and a better basis for future improvement. As a preliminary step, we present our expressions for the currently used precession quantities A;A; zA, in agreement with the MHB corrections to the precession rates, that appear in the IERS Conventions 2000. We then discuss a more sophisticated method for improving the precession model of the equator in order that it be compliant with the IAU 2000A model. In contrast to the first method, which is based on corrections to the t terms of the developments for the precession quantities in longitude and obliquity, this method also uses corrections to their higher degree terms. It is essential that this be used in conjunction with an improved model for the ecliptic precession, which is expected, given the known discrepancies in the IAU 1976 expressions, to contribute in a significant way to these higher degree terms. With this aim in view, we have developed new expressions for the motion of the ecliptic with respect to the fixed ecliptic using the developments from Simon et al. (1994) and Williams (1994) and with improved constants fitted to the most recent numerical planetary ephemerides. We have then used these new expressions for the ecliptic together with the MHB corrections to precession rates to solve the precession equations for providing new solution for the precession of the equator that is dynamically consistent and compliant with IAU 2000. A number of perturbing eects have first been removed from the MHB estimates in order to get the physical quantities needed in the equations as integration constants. The equations have then been solved in a similar way to Lieske et al. (1977) and Williams (1994), based on similar theoretical expressions for the contributions to precession rates, revised by using MHB values. Once improved expressions have been obtained for the precession of the ecliptic and the equator, we discuss the most suitable precession quantities to be considered in order to be based on the minimum number of variables and to be the best adapted to the most recent models and observations. Finally we provide developments for these quantities, denoted the P03 solution, including a revised Sidereal Time expression.

Expressions to implement the IAU 2000 definition of UT1

This paper provides expressions to be used to implement the new definition of UT1 corresponding to the IAU 2000 resolutions either in the new (CEO-based) or classical (equinox-based) transformations between the International Terrestrial Reference System (ITRS) and the Geocentric Celestial Reference System (GCRS). The new expression for Greenwich Sidereal Time (GST) has to be in agreement at the microarcsecond level, for one century, with the IAU 2000 expressions for the Earth Rotation Angle (ERA) and for the quantity s positioning the Celestial Ephemeris Origin (CEO) on the equator of the CIP. The computations of the new expressions using the IAU 2000 precession-nutation model are performed in such a manner as to ensure that there is no discontinuity in UT1 on 1 January 2003 and that there is equivalence of the classical and new transformations between the ITRS and GCRS relative to the rotation about the axis of the CIP when these expressions are used. The equinox offset that is considered in the computations refers to the dynamical mean equinox of J2000.0. The resulting expressions have been included in the IERS Conventions 2000.

Harmonic analysis of the Earth's gravitational field by means of semi-continuous ephemerides of a low Earth orbiting GPS-tracked satellite. Case study: CHAMP

An algorithm for the determination of the spherical harmonic coefficients of the terrestrial gravitational field representation from the analysis of a kinematic orbit solution of a low earth orbiting GPS-tracked satellite is presented and examined. A gain in accuracy is expected since the kinematic orbit of a LEO satellite can nowadays be determined with very high precision, in the range of a few centimeters. In particular, advantage is taken of Newton's Law of Motion, which balances the acceleration vector with respect to an inertial frame of reference (IRF) and the gradient of the gravitational potential. By means of triple differences, and in particular higher-order differences (seven-point scheme, nine-point scheme), based upon Newton's interpolation formula, the local acceleration vector is estimated from relative GPS position time series. The gradient of the gravitational potential is conventionally given in a body-fixed frame of reference (BRF) where it is nearly time independent or stationary. Accordingly, the gradient of the gravitational potential has to be transformed from spherical BRF to Cartesian IRF. Such a transformation is possible by differentiating the gravitational potential, given as a spherical harmonics series expansion, with respect to Cartesian coordinates by means of the chain rule, and expressing zero- and first-order Ferrer's associated Legendre functions in terms of Cartesian coordinates. Subsequently, the BRF Cartesian coordinates are transformed into IRF Cartesian coordinates by means of the polar motion matrix, the precession–nutation matrices and the Greenwich sidereal time angle (GAST). In such a way a spherical harmonic representation of the terrestrial gravitational field intensity with respect to an IRF is achieved. Numerical tests of a resulting Gauss–Markov model document not only the quality and the high resolution of such a space gravity spectroscopy, but also the problems resulting from noise amplification in the acceleration determination process.

Space Gravity Spectroscopy - determination of the Earth’s gravitational field by means of Newton interpolated LEO ephemeris Case studies on dynamic (CHAMP Rapid Science Orbit) and kinematic orbits

Abstract. An algorithm for the (kinematic) orbit analysis of a Low Earth Orbiting (LEO) GPS tracked satellite to determine the spherical harmonic coefficients of the terrestrial gravitational field is presented. A contribution to existing long wavelength gravity field models is expected since the kinematic orbit of a LEO satellite can nowadays be determined with very high accuracy in the range of a few centimeters. To demonstrate the applicability of the proposed method, first results from the analysis of real CHAMP Rapid Science (dynamic) Orbits (RSO) and kinematic orbits are illustrated. In particular, we take advantage of Newton’s Law of Motion which balances the acceleration vector and the gradient of the gravitational potential with respect to an Inertial Frame of Reference (IRF). The satellite’s acceleration vector is determined by means of the second order functional of Newton’s Interpolation Formula from relative satellite ephemeris (baselines) with respect to the IRF. Therefore the satellite ephemeris, which are normally given in a Body fixed Frame of Reference (BRF) have to be transformed into the IRF. Subsequently the Newton interpolated accelerations have to be reduced for disturbing gravitational and non-gravitational accelerations in order to obtain the accelerations caused by the Earth’s gravitational field. For a first insight in real data processing these reductions have been neglected. The gradient of the gravitational potential, conventionally expressed in vector-valued spherical harmonics and given in a Body Fixed Frame of Reference, must be transformed from BRF to IRF by means of the polar motion matrix, the precession-nutation matrices and the Greenwich Siderial Time Angle (GAST). The resulting linear system of equations is solved by means of a least squares adjustment in terms of a Gauss-Markov model in order to estimate the spherical harmonics coefficients of the Earth’s gravitational field.Key words. space gravity spectroscopy, spherical harmonics series expansion, GPS tracked LEO satellites, kinematic

Prediction of the Sidereal Time Distribution of Gravitational Wave Events for Different Detectors

NAUTILUS-EXPLORER coincidences of gravitational wave (GW) events observed during 1998 and 2001 independently reveal the possible excess of events around 4 and 14 hr of sidereal time, exactly where it was predicted for tensor GW sources localized in the Galactic center. The statistical significance of the observed excess is small and needs confirmation. Nevertheless, if one accepts this result, one can predict the distribution of GW events that should be observed by other existing detectors. This gives us a way to confirm or reject the interpretation of these observations as being due to real GW signal. Then, we discuss the methods of analysis in order to facilitate the interpretation. First, we emphasize that the detectors used for coincidence analysis must be compatible, otherwise some coincident events may be lost. Then, we emphasize two important points resulting from the natural modulation of the signal provided by the Earth's rotation: (1) the sidereal time analysis can work with one detector only, without necessarily considering coincidences between two detectors, and (2) a very low signal-to-noise ratio (≈0.5) can be used.

Fractality in high energy cosmic rays

Using EAS data from the EAS-EXC group (EAS plus hadronic calorimeter and nuclear emulsion-X chamber hybrid experiment) on Mount Chacaltaya during the 1990's the fractal properties of the energetic cosmic ray fluxes was investigated. A discrimination in the hadron content of the energetic primaries furnishes two different data samples, the total EAS fluxes and the hadron-less fluxes. The sidereal diurnal variation of the hadron-less EAS time variation shows values of 0.5% with a phase at about 2.29 hr sidereal time. With the help of the Crassberger Procaccia algorithm the fractal dimensions have been investigated of, on the one hand, the differences in arrival times of the hadron-less showers and on the other hand the EAS fluxes time series with an integration time of five min. The obtained fractal dimensions show inconclusive evidence of continuous chaotic component in the data samples investigated.

Determining riometer quiet day curves 1. The matrix method

A number of methods have been proposed for the determination of quiet day curves of riometer recordings of cosmic radio noise in polar regions. Most of these methods are based on the distribution of the recorded intensities, in a given siderial time period, over a number of consecutive days. The method proposed in this paper is based on the filtering, using a low‐pass filter in the Fourier domain, of a discrete two‐dimensional function or matrix. The two dimensions of the matrix are siderial time and day number, with each row of the matrix representing one siderial day. With a low‐pass filter the low frequency Fourier coefficients are retained while the high frequency Fourier coefficients are discarded. The highest Fourier coefficient that is retained is the cutoff frequency of the filter. The proposed method was compared to two existing methods using data obtained from a single broad beam antenna. It was found that the proposed method is less sensitive to noise than the existing methods.

Determining riometer quiet day curves 2. Derivation of filter cutoff frequencies

A method for the determination of riometer quiet day curves which is based on the filtering of a discrete two‐dimensional function or matrix has been proposed. The two dimensions of the matrix are siderial time and day number, with each row of the matrix representing one siderial day. The filtering is done in the Fourier domain using a low‐pass filter. With a low‐pass filter the low frequency Fourier coefficients are retained, while the high frequency Fourier coefficients are discarded. The highest Fourier coefficient that is retained is the cutoff frequency of the filter. In this paper the filter cutoff frequencies are derived directly from the antenna reception pattern as well as from the data itself. A number of methods can be used to infer a cutoff frequency from the data; however, only a number of entropy based methods are investigated in this paper.

New limit on signals of Lorentz violation in electrodynamics.

We describe the results of an experiment to test for spacetime anisotropy terms that might exist from Lorentz violations. The apparatus consists of a pair of cylindrical superconducting cavity-stabilized oscillators operating in the TM010 mode with one axis east-west and the other vertical. Spatial anisotropy is detected by monitoring the beat frequency at the sidereal rate and its first harmonic. We see no anisotropy to a part in 10(13). This puts a comparable bound on four linear combinations of parameters in the general standard model extension, and a weaker bound of < 4 x 10(-9) on three others.