On magnetostatic equilibrium in a stratified atmosphere     

B. C. Low 《Solar physics》1980,65(1):147-165

This is a study of the relationship between a magnetic field and its embedding plasma in static equilibrium in a uniform gravity. The ideal gas law is assumed. A system invariant in a given direction is treated first. We show that an exact integral of the equation for force balance across field lines can be derived in a closed form. Using this integral, exact solutions can be generated freely by integrating directly for the distributions of pressure, density and temperature necessary to keep a given magnetic field in equilibrium. Particular solutions are presented for illustration with the solar atmosphere in mind. Extending the treatment to the general system depending on all three spatial coordinates, we arrive at the general form of a theorem of Parker that a magnetic field in static equilibrium must possess certain symmetries. We derive an equation involving the Euler potentials of the magnetic field stipulating these necessary symmetries. Only those magnetic fields satisfying this equation can be in static equilibrium and for these fields, the endowed symmetries make the construction of exact solutions an essentially two dimensional problem as exemplified by the special case of invariance in a given direction.  相似文献   

Jupiter at five microns     

K.R. Armstrong  R.B. Minton  G.H. Rieke  F.J. Low 《Icarus》1976,29(2):287-298

Maps of Jupiter at 5 um provide detailed information about the complex of emission features at this wavelength. Previous indications of a correlation between infrared sources and visual features are confirmed with a few significant exceptions. The behavior of Jupiter at 5 um is compared with that of other bodies in the outer solar system. Recent observations indicate emission features on Jupiter at other infrared wavelengths.  相似文献   

Post-sunset cooling behavior of the lunar surface     

W. W. Mendell  F. J. Low 《Earth, Moon, and Planets》1972,4(1-2):18-27

Differential infrared flux scans at 22m have been made across the nighttime lunar surface over a range of phases before and after new Moon. The differential chopping technique effectively cancels atmospheric emission in the beam path but records the flux difference between adjacent resolution elements on the lunar disk. The scans show that the brightness temperature gradient across the highlands after sunset is much greater than that across the western maria. The large gradients consistently disappear approximately 3.5 days after sunset. The post-sunset enhancement could be due to surface roughness in the highlands or to a significant surface rock population with a mean size of approximately 0.5 m. The effect can be seen in the 10m measurements of other investigators, but its global nature was not detected in their limited data sets.  相似文献   

The vertical filamentary structures of quiescent prominences     

B. C. Low 《Solar physics》1982,75(1-2):119-131

We present a simple magnetostatic theory of the thin vertical filaments that make up the quiescent prominence plasma as revealed by fine spatial resolution H photographs. A class of exact equilibrium solutions is obtained describing a horizontal row of long vertical filaments whose weights are supported by bowed magnetic field lines. A free function is available to generate different assortments of filament sizes and spacings, as well as different density and temperature variations. The classic Kippenhahn-Schlüter solution for a long sheet without filamentary structures is a particular member of this class of solutions. The role of the magnetic field in supporting and thermally shielding the filament plasma is illustrated. It is found that the filament can have a sharp transition perpendicular to the local field, whereas the transition in the direction of the local field is necessarily diffuse. A consequence of the filamentary structure is that its support by the Lorentz force requires the electric current to have a component along the magnetic field. This electric current flowing into the rarefied region around the prominence can contain substantial energy stored in the form of force-free magnetic fields. This novel feature has implications for the heating and the disruption of prominences.  相似文献   

The Decay of Supersonic and Super-Alfvénic Turbulence in Star-Forming Clouds     

Mordecai-Mark Mac Low  Michael D. Smith  Ralf S. Klessen  Andreas Burkert 《Astrophysics and Space Science》1998,261(1-4):195-196

Supersonic and super-Alfvénic turbulent motions generate an intricate pattern of shock waves through which the turbulence decays. We here illustrate the spatial structure during shock formation and decay. This revised version was published online in July 2006 with corrections to the Cover Date.  相似文献   

Supersonic Ambipolar Diffusion: Estimating the Magnetic Field Strength in Protostellar Outflows     

Michael D. Smith  Mordecai-Mark Mac Low 《Astrophysics and Space Science》1998,261(1-4):191-192

The magnetic field plays a crucial role in star formation. It is involved in rotational braking, collapse braking, outflow formation and jet collimation. Direct observations of the field are difficult. However, the field can be indirectly estimated through the field-cushioned C-shocks which produce strong infrared molecular emission lines. In particular, a high field in the outflows will generate the ‘shock absorber’ signature: very broad H₂lines. Such lines are indeed observed. Here we summarise recent progress in C-shock formation and stability. We demonstrate numerically that the Shock Absorbers are evolutionary and stable. The widths of H₂lines then limit the magnetic field strength. A field of 6 mG is suggested for HH 212. This revised version was published online in July 2006 with corrections to the Cover Date.  相似文献   

Hydrodynamical Simulations of Molecular Dynamics in Supersonic Turbulent Flow     

Georgi Pavlovski  Michael D. Smith  Mordecai–Mark Mac Low  Alexander Rosen 《Astrophysics and Space Science》2004,292(1-4):69-75

Here we present results from simulations of turbulence in star forming environments obtained by coupling three-dimensional hydrodynamical models with appropriate chemical processes. We investigate regimes of decaying high-speed molecular turbulence. Here we analyse PDFs of density for the volume, mass, molecular mass and the energy distribution over the range of scales. We compare our results to those previously obtained for isothermal turbulence and suggest possible explanations.  相似文献   

Densification and grain coarsening of melting snow     

周石硚  中尾正义  桥本重将  坂井亚规子  成田英器  石川信敬 《极地研究(英文版)》2003,14(1)

1　IntroductionSnowdensificationiscriticalforcalculationsinengineering glaciology,snowavalancheforecasting ,springflooding,andotherpracticalaspects.Itisalsoimportantforinterpretingicecoredataincludingthosetakenfromratherwarmsiteswheresurfacelay ersexperiencemelting ,sinceitwouldaffectthechangeofannuallayerthicknesswithtime.Whileextensivestudies(e.g .AndersonandBenson 1 963 ;Bader1 960 ,1 962 ;Koji ma 1 95 4,1 95 5 ,1 95 6,1 95 7,1 95 8,1 95 9,1 964;Keeler 1 967;Gow 1 975 ;MaenoandE binuma 1…  相似文献   

The Craig – Sneyd Analytic Solutions to the Parker Problem     

B. C. Low 《Solar physics》2010,266(2):277-291

This paper follows up on the conclusion by Craig and Sneyd (2005) that the solutions to a linearized magnetostatic problem are counterexamples to the magnetostatic model of Parker (1972), demonstrating a general absence of continuous equilibrium for a magnetic field with an arbitrarily prescribed topology. The analysis presented here shows that Craig and Sneyd had incorrectly rejected an important subset of those solutions in a misunderstanding of the Parker model. The complete set of solutions when correctly interpreted is, in fact, physically consistent with the Parker model. A general discussion of the Parker theory of spontaneous current sheets is given.  相似文献   

Electron content power spectral estimates: Periods of 2 days to $\text{1}\text{2}$ year     

N.C. Low  T.H. Roelofs  P.C. Yuen 《Planetary and Space Science》1975,23(1):133-141

The power spectra of the daily peak electron content measured at Hawaii are estimated via covariance estimations, bivariate autoregressive estimations and fast Fourier transforms for a year of data close to minimum solar activity (1965) and a year of data close to maximum solar activity (1969). The strong peaks about 6 days and 15 days in the 1965 and 1969 power spectra, respectively, suggest an influence of the interplanetary magnetic sector structure on the electron content at low latitude (21·3°N, geographic). The daily solar flux (Sa) at 2800 MHz of 1965 and 1969 are analysed similarly. The decrease in energy content with period range of 3–7 days in the 1969 Sa power spectrum supports the above point of view.  相似文献