The 60-μm extragalactic background radiation intensity, dust-enshrouded active galactic nuclei and the assembly of groups and clusters of galaxies     

A. W. Blain  T. G. Phillips 《Monthly notices of the Royal Astronomical Society》2002,333(1):222-230

  相似文献   

Thermodynamics of selected solar flares as determined from the analysis of the spectra obtained with the RESIK instrument     

B. Sylwester  J. Sylwester  A. Kepa  Z. Kordylewski  K. J. H. Phillips  V. D. Kuznetsov 《Solar System Research》2006,40(2):125-132

The RESIK instrument is an X-ray spectrometer with bent crystals onboard the CORONAS-F satellite. It was used to observe the spectra of solar flares, active regions, and quiet corona. During the period of the instrument’s operation, many spectra were collected in four energy channels covering the wavelength range from 3.2 to 6.1 Å. For the present analysis, we selected solar flares of various X-ray classes (B, C, and M in the GOES notation), which were observed during moderate level of solar activity (from January to March 2003). The analysis of the RESIK spectra fulfilled with different techniques allowed us to determine the temperature, emission measure, and temperature distribution of the differential emission measure, as well as to examine their time variability.  相似文献   

Dust masses and abundances in planetary nebulae: likely strong elemental depletion in low-abundance sources     

J. P. Phillips 《Monthly notices of the Royal Astronomical Society》2007,381(1):117-124

An analysis is undertaken of the relation between dust/gas mass ratios and elemental abundances within planetary nebulae (PNe). It is found that M _DUST/ M _GAS is broadly invariant with abundance, and similar to the values observed in asymptotic giant branch (AGB)-type stars. However, it is noted that the masses of dust observed in low-abundance PNe are similar to the masses of heavy elements observed in the gas phase. This is taken to imply that levels of elemental depletion must be particularly severe, and extend to many more species than have been identified so far. In particular, given that levels of C and O depletion are likely to be large, then this probably implies that species such as Fe, S, Si and Mg are depleted as well. There is already evidence for depletion of Fe, Si and Mg in individual PNe. It follows that whilst quoted abundances may accurately reflect gas-phase conditions, they are likely to be at variance with intrinsic abundances in low Z _N nebulae.
Finally, we note that there appears to be a variation in dust/gas mass ratios with galactocentric distance, with gradient similar to that observed for several elemental abundances. This may represent direct evidence for a correlation between dust/gas mass ratios and nebular abundances.  相似文献   

The inception of novae transition zone oscillations     

J. P. Phillips  M. J. Selby 《Astrophysics and Space Science》1977,49(2):339-348

The nature of semi-regular oscillations in the transition zones of certain novae is discussed. It is found that hydrostatic collapse following a reduction of radiative support for the photospheric layers is a likely explanation of transition zone inception.  相似文献   

The cooling of flare produced plasmas in the solar corona     

J. L. Culhane  J. F. Vesecky  K. J. H. Phillips 《Solar physics》1970,15(2):394-413

Solar flare X-rays, at energies less than 10 keV, are emitted by hot plasmas located in the corona. Three plasma cooling models are examined in detail. The cooling of the electrons by Coulomb collisions with ions at a lower temperature would require the observed material to occupy very large volumes. Cooling could take place by conduction or by radiation and observations are proposed which would allow the dominant cooling mechanism to be established.On leave during a portion of this work as University Research Fellow in Astronomy, University of Leicester, England.  相似文献   

The radiosonde intercomparison SONDEX spring 1981, Payerne     

Hans Richner  Peter D. Phillips 《Pure and Applied Geophysics》1982,120(5-6):852-1198

  相似文献   

Ar/Ar thermochronology of the Kampa Dome, southern Tibet: Implications for tectonic evolution of the North Himalayan gneiss domes     

Mark Quigley  Yu Liangjun  Liu Xiaohan  Christopher J.L. Wilson  Mike Sandiford  David Phillips 《Tectonophysics》2006,421(3-4):269-297

Structural and thermochronological studies of the Kampa Dome provide constraints on timing and mechanisms of gneiss dome formation in southern Tibet. The core of Kampa Dome contains the Kampa Granite, a Cambrian orthogneiss that was deformed under high temperature (sub-solidus) conditions during Himalayan orogenesis. The Kampa Granite is intruded by syn-tectonic leucogranite dikes and sills of probable Oligocene to Miocene age. Overlying Paleozoic to Mesozoic metasedimentary rocks decrease in peak metamorphic grade from kyanite + staurolite grade at the base of the sequence to unmetamorphosed at the top. The Kampa Shear Zone traverses the Kampa Granite — metasediment contact and contains evidence for high-temperature to low-temperature ductile deformation and brittle faulting. The shear zone is interpreted to represent an exhumed portion of the South Tibetan Detachment System. Biotite and muscovite ⁴⁰Ar/³⁹Ar thermochronology from the metasedimentary sequence yields disturbed spectra with 14.22 ± 0.18 to 15.54 ± 0.39 Ma cooling ages and concordant spectra with 14.64 ± 0.15 to 14.68 ± 0.07 Ma cooling ages. Petrographic investigations suggest disturbed samples are associated with excess argon, intracrystalline deformation, mineral and fluid inclusions and/or chloritization that led to variations in argon systematics. We conclude that the entire metasedimentary sequence cooled rapidly through mica closure temperatures at  14.6 Ma. The Kampa Granite yields the youngest biotite ⁴⁰Ar/³⁹Ar ages of  13.7 Ma immediately below the granite–metasediment contact. We suggest that this age variation reflects either varying mica closure temperatures, re-heating of the Kampa Granite biotites above closure temperatures between 14.6 Ma and 13.7 Ma, or juxtaposition of rocks with different thermal histories. Our data do not corroborate the “inverse” mica cooling gradient observed in adjacent North Himalayan gneiss domes. Instead, we infer that mica cooling occurred in response to exhumation and conduction related to top-to-north normal faulting in the overlying sequence, top-to-south thrusting at depth, and coeval surface denudation.  相似文献   

Reconstruction of long-term precipitation records for Edinburgh: an examination of the mechanisms responsible for temporal variability in precipitation     

N. Macdonald  I. D. Phillips  J. Thorpe 《Theoretical and Applied Climatology》2008,92(3-4):141-154

Summary Recent dry years (combined dry winter and summer months) within the UK (2005 and 2006) have enhanced concerns relating to long term water resources and future water provision in large conurbations. This paper examines the mechanisms responsible for precipitation variability for five different areas in Edinburgh (precipitation regions) using composite historic precipitation records for the period 1861–2005. Trend analysis and principal component analysis (PCA) were undertaken to examine precipitation variability over time and space. Annual correlation co-efficients were derived for relationships between precipitation areas, atmospheric–oceanographic variations and geographic parameters. Stepwise regression models were constructed to specify annual precipitation, through atmospheric variations, for each of the precipitation areas. Significant downward trends in precipitation (p < 0.05) were noted in two out of the five precipitation areas, with one principal component representing precipitation variability over Edinburgh and the Pentland Hills. Precipitation variability is best explained by fluctuations in pressure, altitude and proximity to coast. Precipitation trends cannot be explained by changes in atmospheric circulation patterns. Authors’ addresses: N. Macdonald, Department of Geography, University of Liverpool, Liverpool L69 7ZT, United Kingdom; I. D. Phillips, J. Thorpe, School of Geography, Earth and Environmental Sciences, University of Birmingham, Edgbaston B15 2TT, United Kingdom.  相似文献   

Wind-swept clouds and possible triggered star formation associated with the supernova remnant G357.7+0.3     

J. P. Phillips  G. Ramos-Larios  J. A. Perez-Grana 《Monthly notices of the Royal Astronomical Society》2009,397(3):1215-1227

We present evidence for interaction between the supernova remnant (SNR) G357.7+0.3 and nearby molecular clouds, leading to the formation of wind-swept structures and bright emission rims. These features are not observed at visual wavelengths, but are clearly visible in mid-infrared mapping undertaken using the Spitzer Space Telescope . Analysis of one of these clouds, the bright cometary structure G357.46+0.60, suggests that it contains strong polycyclic aromatic hydrocarbon emission features in the 5.8 and 8.0 μm photometric bands, and that these are highly variable over relatively small spatial scales. The source is also associated with strong variations in electron density; a far-infrared continuum peak associated with dust temperatures of ∼30 K; and has previously been observed in the 1720 MHz maser transition of OH, known to be associated with SNR shock excitation of interstellar clouds. This source also appears to contain a young stellar object (YSO) within the bright rim structure, with a steeply rising spectrum between 1.25 and 24 μm. If the formation of this star has been triggered recently by the SNR, then YSO modelling suggests a stellar mass  ∼5–10 M_⊙  , and luminosity   L _YSO∼10²–2 × 10³ L_⊙  .
Finally, it is noted that a further, conical emission region appears to be associated with the Mira V1139 Sco, and it is suggested that this may represent the case of a Mira outflow interacting with a SNR. If this is the case, however, then the distance to the SNR must be ∼half of that determined from CS   J = 2–1  and 3–2 line radial velocities.  相似文献   

Science with ASKAP     

S. Johnston  R. Taylor  M. Bailes  N. Bartel  C. Baugh  M. Bietenholz  C. Blake  R. Braun  J. Brown  S. Chatterjee  J. Darling  A. Deller  R. Dodson  P. Edwards  R. Ekers  S. Ellingsen  I. Feain  B. Gaensler  M. Haverkorn  G. Hobbs  A. Hopkins  C. Jackson  C. James  G. Joncas  V. Kaspi  V. Kilborn  B. Koribalski  R. Kothes  T. Landecker  A. Lenc  J. Lovell  J.-P. Macquart  R. Manchester  D. Matthews  N. McClure-Griffiths  R. Norris  U.-L. Pen  C. Phillips  C. Power  R. Protheroe  E. Sadler  B. Schmidt  I. Stairs  L. Staveley-Smith  J. Stil  S. Tingay  A. Tzioumis  M. Walker  J. Wall  M. Wolleben 《Experimental Astronomy》2008,22(3):151-273

  相似文献