bluuebunny/crossref_metadata_2025_split huggingface dataset:
Does Khaṛī Bolī mean nothing more than Rustic Speech ?
Authors: Bailey T. Grahame 
Published: January 2010

THIS question arises out of some remarks made by Professor Abdul Haq of the Osmaniya University, Hyderabad, Deccan, who, criticizing views on Khaṛī Bolī (=KB) which I had expressed in my Hist, of Urdu Lit., pp. 5, 8, 9, 13, said :—hamẽ is se hūī ki ḍākṭar ṣāḥab ne is ko rafa‘ kīā hai, lekin aṣl mẽ yeh bhī mubtilā haī: khaṛī aur kharī kā farq inhõ ne bahut ṣaḥiḥ batāeā. hai, lekin ma‘ne taqrīban vohī rakkhe haī jo kharī ke haī, ya‘ne murawaja, ‘ām, mustanad (standard) zabān ; aur dūsrā gaẓab kīā hai ki Khaṛī Bolī ko ek zabān qarār dīā hai, aur us kī do batāī haī, ek Hindī aur dūsrī Urdū … Khaī Bolī ke ma‘ne Hindostān mẽ ‘ām par gãvārī bolī ke haī jise Hindostān kā, bacca bacca jāntā, hai; voh na koī khāṣ zabān hai, aur na zabān kī koī (Urdu, July, 1933, p. 590.)
Hāritī and the chronology of the Kuṣāṇas
Authors: Bivae A. D. H. 
Published: January 2010

The view has more than once been mooted amongst archaeologists, though dissenting voices have frequently made themselves heard, that the art of the ‘Graeco-Buddhist’ School of Gandhāra is contemporary with the zenith of the Kuṣāṇa dynasty under the rulers Kaniṣka, Huviṣka, and perhaps Vāsudeva. A further analysis is naturally required to convert this proposition into terms of absolute chronology. Yet the basic thesis is one that would find justification in an argument developed by Ibn Khaldūn in his masterpiece of historical theory, theMuqaddima:‘The monuments of a dynasty are its buildings and large (edifices). They are proportionate to the original power of the dynasty. They can materialize only when there are many workers, and united action and co-operation. When a dynasty is large and far-flung, with many provinces and subjects, workers are very plentiful, and can be brought together from all sides and regions. Thus even the largest monument can materialize’.
Some aspects of the Anglo-Russian Convention and its working in Persia, 1907–14—II
Authors: Greaves Rose Louise 
Published: January 2010

The Americans arrived (May 1911) to find Tehran in a turmoil of political excitement. In February the Minister of Finance, who had been a leading figure in the constitutional movement, had been assassinated by Russian subjects on his way home from attending the Majlis. This was followed by another political murder in Tehran later in February—again undertaken by Russian nationals. Since Russia retained the right of jurisdiction over her own subjects in Persia the murderers had to be hunded over to the Russian government. The situation the Americans found has been described by one of the members of the mission in a latter to President Taft. He wrote:‘Pursuant to your kind request to keep you informed of our progress in Persia, the following statement of experiences and conditions may be of interest, especially in view of the recent return of the exiled Shah, Mohammed Ali, and the near approach of civil war which now seems inevitable, as the result of foreign intrigues. The entire country is in the most complete state of anarchy possible to imagine, and the government—if such it can be called—is of the opera bouffe variety, fit to adorn any stage without alteration of a single feature. Civic corruption exists to an extent beyond the limits of the wildest imagination, and is so widespread that an honest official, high or low, is almost unknown. No laws exist for the punishment of official crimes, and as the Oriental system of bribery for the consummation of any purpose whatsoever has existed since time immemorial, the natural result is beyond description.
Arya II
Authors: Bailey H. W. 
Published: January 2010

A Buddhist practice existed whereby adānapati, patron, had a manuscript of a Buddhist religious text copied, into which at the appropriate place his personal name was inserted with Sanskrit inflexion. In the Buddhist SanskritSitātapatra-sūtra, the ‘Book of the white umbrella’, Stein manuscript S 2529, two personal names are inserted. In lines 45–6 occursaṣṭānā mahāgrrahāṇā vaidhvasanakara hu ttrū 〈rakṣa rakṣa〉 mama vaṣayānasya‘O destroyer of the eight great ravishers,hūṃ trūṃ. Protect, protect me Yaṣayāna’. In lines 48, 70, 88, 117 the name is Sīdyākaraca. Here we read:48auma svasta〈ka〉ra bavattū mama sīdyākaracasya70rakṣa rakṣa mama sīdyākaracasya:88ye ke cai salvā mama sīdyākaracasya ∥117:rakṣa rakṣa mama sīdyākaracasya:Instead of a name in line 122 occurs the wordīthanāmasya‘of so-and-so’.
Beyond the standard IAU framework
Authors: Kopeikin Sergei 
Published: January 2010

AbstractWe discuss three conceivable scenarios of extension and/or modification of the IAU relativistic resolutions on time scales and spatial coordinates beyond the Standard IAU Framework. These scenarios include: (1) the formalism of the monopole and dipole moment transformations of the metric tensor replacing the scale transformations of time and space coordinates; (2) implementing the parameterized post-Newtonian formalism with two PPN parameters – β and γ; (3) embedding the post-Newtonian barycentric reference system to the Friedman-Robertson-Walker cosmological model.
Units of measurement in relativistic context
Authors: Guinot Bernard 
Published: January 2010

AbstractIn the Newtonian approximation of General Relativity, employed for the dynamical modelling in the solar system, the coordinates have the dimension of time and length. As these coordinates are close to their Newtonian counterpart, the adherence to the rules of the Quantity Calculus does not raise practical difficulties: the second and the metre should be used as their units, in an abstract conception of these units. However, the scaling of coordinate times, applied for practical reasons, generates controversies, because there is a lack of information about the metrics to which they pertain. Nevertheless, it is not satisfactory to introduce specific units for these scaled coordinate times.
Models and nomenclature in Earth rotation
Authors: Capitaine Nicole 
Published: January 2010

AbstractThe celestial Earth's orientation is required for many applications in fundamental astronomy and geodesy; it is currently determined with sub-milliarcsecond accuracy by astro-geodetic observations. Models for that orientation rely on solutions for the rotation of a rigid Earth model and on the geophysical representation of non-rigid Earth effects. Important IAU 2000/2006 resolutions on reference systems have been passed (and endorsed by the IUGG) that recommend a new paradigm and high accuracy models to be used in the transformation from terrestrial to celestial systems. This paper reviews the consequences of these resolutions on the adopted Earth orientation parameters, IAU precession-nutation models and associated nomenclature. It summarizes the fundamental aspects of the current IAU precession-nutation models and reports on the consideration of General Relativity (GR) in the solutions. This shows that the current definitions and nomenclature for Earth's rotation are compliant with GR and that the IAU precession-nutation is compliant with the IAU 2000 definition of the geocentric celestial reference system in the GR framework; however, the underlying Earth's rotation models basically are Newtonian.
Gravitational light deflection, time delay and frequency shift in Einstein-Aether theory
Authors: Tang Kai , Huang Tian-Yi , Tang Zheng-Hong 
Published: January 2010

AbstractEinstein-Aether gravity theory has been proven successful in passing experiments of different scales. Especially its Eddington parameters β and γ have the same numerical values as those in general relativity. Recently Xie and Huang (2008) have advanced this theory to a second post-Newtonian approximation for an N-body model and obtained an explicit metric when the bodies are point-like masses. This research considers light propagation in the above gravitational field, and explores the light deflection, time delay, frequency shift etc. The results will provide for future experiments in testing gravity theories.
A relativistic motion integrator: numerical accuracy and illustration with BepiColombo and Mars-NEXT
Authors: Hees A. , Pireaux S. 
Published: January 2010

AbstractToday, the motion of spacecraft is still described by the classical Newtonian equations of motion plus some relativistic corrections. This approach might become cumbersome due to the increasing precision required. We use the Relativistic Motion Integrator (RMI) approach to numerically integrate the native relativistic equations of motion for a spacecraft. The principle of RMI is presented. We compare the results obtained with the RMI method with those from the usual Newton plus correction approach for the orbit of the BepiColombo (around Mercury) and Mars-NEXT (around Mars) orbiters. Finally, we present a numerical study of RMI and we show that the RMI approach is relevant to study the orbit of spacecraft.
Relativistic aspects of the JPL planetary ephemeris
Authors: Folkner W. M. 
Published: January 2010

AbstractThe orbits of the planets as represented by the JPL planetary ephemerides are now primarily determined by radio tracking of spacecraft. Analysis of the data and propagation of the orbits relies on an internally consistent set of equations of motion and propagation of radio signals including relativistic effects at the centimeter level. The planetary ephemeris data set can be used to test some aspects of the underlying theory such as estimates of PPN parameters γ and β, time variation in the gravitational constant G, rotation of the solar system relative to distant objects (Mach's principle), and place stringent limits on the possible violation of the inverse-square law.
Gravity tests with INPOP planetary ephemerides
Authors: Fienga A. , Laskar J. , Kuchynka P. , Leponcin-Lafitte C. , Manche H. , Gastineau M. 
Published: January 2010

AbstractWe present here several gravity tests made with the latest INPOP08 planetary ephemerides. We first propose two methods to estimate the PPN parameter β and its correlated value, the Sun J2, and we discuss the correlation between the Sun J2 and the mass of the asteroid ring. We estimate a possible advance in the planet perihelia. We also show that no constant acceleration larger than 1/4 of the Pioneer anomaly is compatible with the observed motion of the planets in our Solar System.
Probing general relativity with radar astrometry in the inner solar system
Authors: Margot Jean-Luc , Giorgini Jon D. 
Published: January 2010

AbstractWe describe a long-term program designed to obtain and interpret high-precision radar range measurements of a number of near-Earth objects (NEOs) that have trajectories reaching deep inside the gravitational well of the Sun. Objects in our sample have perihelion shift rates 1.5 to 2.5 times that of (1566) Icarus (10″/cy) and span a wide range of inclinations and semi-major axes, allowing for an unambiguous separation of general relativistic and solar oblateness effects. Four objects have been observed at Arecibo on at least two apparitions since 2000, with typical uncertainties of a few hundred meters. Within the next three years, we anticipate securing a total of 15 observations of 5 different NEOs. This program is expected to provide a purely dynamical measurement of the oblateness of the Sun (J2 at the 10−8 level) and to constrain the Eddington parameter β at the 10−4 level. Although our objects are selected to minimize Yarkovsky orbital drift, we also anticipate measuring Yarkovsky drift rates, which are orthogonal to the GR and J2 signatures.
Open loop doppler tracking in Chinese forthcoming Mars mission
Authors: Shang Kun , Ping Jinsong , Dai Chunli , Jian Nianchuan 
Published: January 2010

AbstractUsing the radio telescopes in Chinese VLBI Network and the K5/VSSP32 VLBI system of NICT in Japan, we have developed algorithms that can extract open loop Doppler information from the Chang'E-1 and Mars Express radio tracking data. Our latest results indicate the Doppler accuracy of open loop three-way Doppler is about 1mm/s in 1 second integration time, relative to a 8.4GHz carrier. In the forthcoming joint Russian-Chinese Martian mission in 2009, the current software algorithms and hardware performance will be improved, and we will attempt to use the high precision Doppler shift and phase information to test gravitation theories.
Pulsar timing array projects
Authors: Hobbs G. 
Published: January 2010

AbstractPulsars are amongst the most stable rotators known in the Universe. Over many years some millisecond pulsars rival the stability of atomic clocks. Comparing observations of many such stable pulsars may allow the first direct detection of gravitational waves, improve the Solar System planetary ephemeris and provide a means to study irregularities in terrestrial time scales. Here we review the goals and status of current and future pulsar timing array projects.
Observing a black hole event horizon: (sub)millimeter VLBI of Sgr A*
Authors: Fish Vincent L. , Doeleman Sheperd S. 
Published: January 2010

AbstractVery strong evidence suggests that Sagittarius A*, a compact radio source at the center of the Milky Way, marks the position of a super massive black hole. The proximity of Sgr A* in combination with its mass makes its apparent event horizon the largest of any black hole candidate in the universe and presents us with a unique opportunity to observe strong-field GR effects. Recent millimeter very long baseline interferometric observations of Sgr A* have demonstrated the existence of structures on scales comparable to the Schwarzschild radius. These observations already provide strong evidence in support of the existence of an event horizon. (Sub)Millimeter VLBI observations in the near future will combine the angular resolution necessary to identify the overall morphology of quiescent emission, such as an accretion disk or outflow, with a fine enough time resolution to detect possible periodicity in the variable component of emission. In the next few years, it may be possible to identify the spin of the black hole in Sgr A*, either by detecting the periodic signature of hot spots at the innermost stable circular orbit or parameter estimation in models of the quiescent emission. Longer term, a (sub)millimeter VLBI “Event Horizon Telescope” will be able to produce images of the Galactic center emission to the see the silhouette predicted by general relativistic lensing. These techniques are also applicable to the black hole in M87, where black hole spin may be key to understanding the jet-launching region.
Global astrometric sphere reconstruction in Gaia: challenges and first results of the Verification Unit
Authors: Vecchiato Alberto , Abbas Ummi , Bucciarelli Beatrice , Lattanzi Mario G. , Morbidelli Roberto 
Published: January 2010

AbstractGaia will estimate the astrometric and physical data of approximately one billion objects. The core of this process, the global sphere reconstruction, is represented by the reduction of a subset of these objects, which will constitute the largest and most precise catalog of absolute astrometry in the history of Astronomy, and will put General Relativity to test by estimating the PPN parameter γ with unprecedented accuracy. As the Hipparcos mission showed, and as it is natural for all kind of absolute measurements, possible errors in the data reduction can hardly be identified at the end of the processing, and can lead to systematic errors in all the works which will use these results. In order to avoid such kind of problems, a Verification Unit was established by the Gaia Data Processing and Analysis Consortium (DPAC). One of its jobs is to implement and perform an independent global sphere reconstruction, parallel to the baseline one, to compare the two results, and to report any significant difference.
Perspective acceleration and gravitational redshift. Measuring masses of individual white dwarfs using Gaia + SIM astrometry
Authors: Anglada-Escudé Guillem , Debes John 
Published: January 2010

AbstractAccording to current plans, the SIM/NASA mission will be launched just after the end of operations for the Gaia/ESA mission. This is a new situation which enables long term astrometric projects that could not be achieved by either mission alone. Using the well-known perspective acceleration effect on astrometric measurements, the true heliocentric radial velocity of a nearby star can be measured with great precision if the time baseline of the astrometric measurements is long enough. Since white dwarfs are compact objects, the gravitational redshift can be quite large (40–80 km/s), and is the predominant source of any shift in wavelength. The mismatch of the true radial velocity with the spectroscopic shift thus leads to a direct measure of the Mass–Radius relation for such objects. Using available catalog information about the known nearby white dwarfs, we estimate how many masses/gravitational redshift measurements can be obtained with an accuracy better than 2%. Nearby white dwarfs are relatively faint objects (10 < V < 15), which can be easily observed by both missions. We also briefly discuss how the presence of a long period planet can mask the astrometric signal of perspective acceleration.
Space astrometry with the Joint Milliarcsecond Astrometry Pathfinder
Authors: Hennessy Gregory S. , Gaume Ralph 
Published: January 2010

AbstractThe Joint Milliarcsecond Astrometry Pathfinder Survey (JMAPS) is a small, space-based, all sky, visible wavelength, astrometric and photometric survey mission for 0ththrough 14thI-band magnitude stars with a planned 2013 launch. The primary objective of the JMAPS mission is the generation of an astrometric star catalog with 1 milliarcsecond (mas) positional accuracy or better and photometry to the 1% accuracy level or better at 1stto 12thmag. A 1-mas all–sky survey will have a significant impact on our current understanding of galactic and stellar astrophysics. JMAPS will improve our understanding of the origins of nearby young stars, provide insight into the dynamics of star formation regions and associations, investigate the dynamics and membership of nearby open clusters.
Two cylindrical masses in orbit for the test of the equivalence principle
Authors: Chhun Ratana , Touboul Pierre , Lebat Vincent 
Published: January 2010

AbstractTwo pairs of solid test-masses have been considered to perform in space the test of the universality of free fall with an accuracy of at least 10−15. These cylindrical masses are precisely at the heart of the MICROSCOPE mission instrument comprising two differential electrostatic accelerometers. These masses shall exhibit material quality, shapes, positions and alignments in regard to stringent experimental requirements. Indeed the space experiment is based on the control of the two masses submitted to the same gravity acceleration along the same orbit at 810 km altitude with an accuracy of 10−11 m. Thus effects of Earth and satellite gravity gradients shall be contained as well as any other disturbances of the mass motions induced by their magnetic susceptibility or electrical dissymmetries, by outgassing of the materials or radiation emissivity. Furthermore, the electrostatic levitation of the two masses depends dramatically on the mass shapes and electrical properties in particular for the definition of the sensitive axes orientation. All these aspects will be presented from the mass characteristics to the space MICROSCOPE experiment performance.
Modelling and simulation of the space mission MICROSCOPE
Authors: Bremer Stefanie , List Meike , Selig Hanns , Lämmerzahl Claus 
Published: January 2010

AbstractThe French space mission MICROSCOPE aims at testing the weak Equivalence Principle (EP) with an accuracy of 10−15. The payload, which is developed and built by the French institute ONERA consists of two high-precision capacitive differential accelerometers. The detection of the test mass movement and their control is done via a complex electrode system. The German department ZARM is member of the MICROSCOPE performance team. In addition to drop tower tests, mission simulations and the preparation of the mission data evaluation are realized in close cooperation with the French partners CNES, ONERA and OCA. Therefore a comprehensive simulation of the real system including the science signal and all error sources is built for the development and testing of data reduction and data analysis algorithms to extract the EP violation signal. In this context the focus lays on the correct modeling of the environmental disturbances. Currently new effort to study the influence of the solar radiation and the Earth albedo to the MICROSCOPE mission scenario is underway.
Microscope – A space mission to test the equivalence principle
Authors: List Meike , Selig Hanns , Bremer Stefanie , Lämmerzahl Claus 
Published: January 2010

AbstractMICROSCOPE is a ESA/CNES space mission for testing the validity of the weak equivalence principle. The mission's goal is to determine the Eötvös parameter η with an accuracy of 10−15. The French space agency CNES is responsible for designing the satellite which is developed and produced within the Myriade series. The satellite's payload T–SAGE (Twin Space Accelerometer for Gravitation Experimentation) consists of two high–precision capacitive differential accelerometers and is developed and built by the French institute ONERA.As a member of the MICROSCOPE performance team, the German department ZARM performs free fall tests of the MICROSCOPE differential accelerometers at the Bremen drop tower. The project's concepts and current results of the free fall tests are shortly presented.
New precise method for accurate modeling of thermal recoil forces
Authors: Rievers Benny , Lämmerzahl Claus 
Published: January 2010

AbstractThe exact modeling of external and internal perturbations acting on spacecraft becomes increasingly important as the scientific requirements become more demanding. Disturbance models included in orbit determination and propagation tools need to be improved to account for the needed accuracy. At ZARM (Center of Applied Space Technology and Microgravity) algorithms for the simulation and analysis of thermal perturbations have been developed. The applied methods are based on the inclusion of the actual spacecraft geometry by means of Finite Element (FE) models in the calculation of the disturbance forces. Thus the modeling accuracy is increased considerably and also housekeeping and sensor data can be included in the calculations. Preliminary results for a test case geometry of the Pioneer 10/11 mission are presented and discussed with respect to the Pioneer anomaly. It is shown that thermal effects cannot be neglected for the magnitude scale of the observed anomalous effect.