AVIAN NESTING HABITS AND VEGETATION STRUCTURE     

Kathleen C. Parker 《The Professional geographer》1987,39(1):47-58

Discriminant analysis is used to identify relationships between vegetation structure and nesting behavior in 78 breeding bird communities in North America. Results indicated that bird communities associated with structurally similar vegetation exhibited similar arrays of nesting habits despite their geographical separation. Tree-cavity, intermediate-cup, and high-cup nesters dominated forests and woodlands; ground-cup and ground-scrape nesters dominated grasslands; and low-cup nesters dominated desert, scrub, and some woodland sites. These functional relationships are distinct from previously reported continental scale relationships between avian feeding habits and gross vegetation structure. Links between nesting behavior and vegetation structure provide us, as geographers, with a means for placing birds into a physical landscape perspective.  相似文献   

The nature of the sunspot phenomenon     

Parker  E. N. 《Solar physics》1974,36(2):249-274

Heat transport in the Sun is describable by a Fokker-Planck, or diffusion, transfer equation. A study of the general character of the solutions of the transfer equation shows that the inhibition of convective transport beneath the photosphere produces a photospheric dark ring surrounded by a bright ring, or at best, a dark area surrounded by a bright ring. The mean temperature beneath the sunspot is unavoidably above normal, so that the enhanced gas pressure would disperse, rather than concentrate, the magnetic field. Hence we conclude that the inhibition of convection cannot be the cause of a sunspot.We suggest, instead, that a sunspot is a region of enhanced, rather than inhibited, energy transport and emissivity. The magnetic field of the sunspot causes a dynamical overstability in the outer thousand km of the convective zone, generating copious fluxes of hydromagnetic waves, which propagate rapidly out of the region along the magnetic field. We suggest that this heat engine is so efficient as to convert at least three fourths of the heat flux into waves. Solutions of the heat transport equation in the presence of a heat sink automatically resemble the observed sunspot, including a dark interior, a sharp transition at the edge of the umbra, and an extended grey area around the outside, the penumbra. The mean temperature is reduced, causing the observed concentration of the magnetic field.The enhanced radiation is in the form of hydromagnetic waves, which do not appear in ordinary photographs, but which light up the sky over the sunspot in a manner conspicuous in any UV or X-ray picture. In this respect, then, a sunspot is effectively a hole in the Sun, extending down to temperatures of 2 × 10⁴ K or more.This work was supported in part by the National Aeronautics and Space Administration under Grant NGL 14-001-001.  相似文献   

    

I. Lerche  E. N. Parker 《Astrophysics and Space Science》1970,8(1):140

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BIOGEOGRAPHY: RESEARCH OPPORTUNITIES FOR GEOGRAPHERS     

Thomas R. Vale  Albert J. Parker 《The Professional geographer》1980,32(2):149-157

The authors of this paper suggest several themes in biogeography worthy of increased research attention by geographers: human impacts on biota, disturbance ecology, and certain aspects of biota-environment interactions. Researchers must gain a firmer command of biological as well as geographical concepts and approaches if biogeography is to join geomorphology and climatology in developing a true geography of environments.  相似文献   

Volatile emission on the moon; Possible sources and release mechanisms     

Friesen  Larry Jay 《Earth, Moon, and Planets》1975,13(4):425-430

Evidence for very recent emission of volatiles on the Moon is primarily of four types: (1) transient lunar optical events observed by Earth-based astronomers; (2) excursions on Apollo SIDE and mass spectrometer instruments; (3) localized Rn²²²/Po²¹⁰ enhancements on the lunar surface detected by Apollo 15 and 16 orbital alpha spectrometers; (4) presence in lunar fines of retrapped Ar⁴⁰ and other volatiles. Available evidence indicates that the release rate of volatile substances into the lunar atmosphere is not steady, but instead sporadic and episodic. Rn²²²/Po²¹⁰ anomalies are at locations that are among those from which transient events have most often been reported (edges of maria, certain specific craters), and are probably related to them. Volatiles emitted at maria rims may originate in the Moon's fluid core, reaching the surface through deep cylindrical fault systems that ring the maria borders. The sources of volatiles emitted at craters such as Aristarchus or Tsiolkovsky, which possess floors which are cracked or filled with dark lava and possess central peaks, are more likely to be local pockets of magma or trapped gas at shallower depths. The volatiles are produced directly by radioactive decay (He⁴, Ar⁴⁰, Rn) and by heating (other volatiles). The release by heating can occur either during melting or by ‘bakeout’ of unmelted materials. Release of gas into the lunar atmosphere is probably triggered by buildup of its own pressure. This may be assisted by tidal forces exerted on the Moon by the Earth. In addition to independent release, volatile emission is also expected to accompany other lunar activity, such as ash flows, if any lunar volcanism is presently active.

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The rings of Uranus: Occultation profiles from three observatories     

J.L. Elliot  J.H. Elias  R.G. French  Jay A. Frogel  W. Liller  K. Matthews  K.J. Meech  D.J. Mink  P.D. Nicholson  B. Sicardy 《Icarus》1983,56(2):202-208

Occultation profiles for the nine confirmed Uranian rings obtained from Las Campanas, the European Southern Observatory, and Cerro Tololo on 15–16 August 1980 are compared. The α ring shows a “double-dip” structure; the η ring shows a broad and narrow component (similar to Saturn's F ring); and the ε ring shows six features that appear in the data from all three observatories. Diffraction fringes appear at the edges of several of the occultation profiles.  相似文献   

Minchinia nelsoni (MSX) infections in the James River seed-oyster area and their expulsion in spring     

Jay D. Andrews 《Estuarine, Coastal and Shelf Science》1983,16(3):255-269

Spread of a new oyster disease caused by Minchinia nelsoni (MSX) in lower Chesapeake Bay in 1959–1960 threatened Virginia's James River seed area. Infections appeared in the lower half of the seed area in 1960 and 1961, but few oysters died from the disease and infections were eliminated by oysters in April-May the following spring. Distribution of the disease in controlled broadly by low salinities that inhibit development of infections and allow oysters to discharge plasmodia. Penetrations of the seed area occurred in dry and wet years, but mortalities occurred only in 1964 and 1980, both years of low precipitation. Little mortality was caused by transplanting infected seed oysters to other rivers because only low-salinity grounds were planted after 1959–1960 when severe mortalities occurred in areas of high salinities. In most years, infections were minimal in the seed area and other estuaries where salinities do not exceed 15–20‰ in late summer and fall. Salinities <10‰ prevailed in most of the seed area when oysters expelled the pathogen in early spring.  相似文献   

The existence of a region inaccessible to magneto-telluric sounding     

Robert L. Parker 《Geophysical Journal International》1982,68(1):165-170

Summary. The exponential attenuation of fluctuating electromagnetic fields suggests that practical magneto telluric measurements may be uninformative about the electrical conductivity at sufficiently great depths. This notion can be made precise for one-dimensional systems. Below a critical depth the conductivity function may be chosen freely without affecting the consistency of the model with the data. This depth is readily computable with quadratic or linear programming techniques and does not rely upon linearization of the equations.  相似文献   

Spectral observations of spicules at two heights in the solar chromosphere     

Jay M. Pasachoff  Robert W. Noyes  Jacques M. Beckers 《Solar physics》1968,5(2):131-158

An observational program at the Sacramento Peak Observatory in 1965 provided high-dispersion spectra of the solar chromosphere in several spectral regions simultaneously. These regions included various combinations of the spectral lines Hα, Hβ and H?, the D₃-line of Hei, the infrared triplet of Oi, and the H- and K-lines and the infrared triplet of Caii. With the use of an image slicer the observations were made simultaneously at two heights in the solar chromosphere separated by several thousand kilometers. From these data we draw the following conclusions:

1. Emission of different lines arises in the same chromospheric features. The intensity ratio of lines of different elements varies significantly from spicule to spicule. For the H- and K-lines of ionized calcium, this ratio remains constant, independent of wavelength throughout the line, overall intensity, and height in the chromosphere. Two rare-earth lines in the wing of the H-line show no spicular structure at all.
2. The line-of-sight velocities of many features reverse as a function of time, although most spicules show velocities in only one direction. The simultaneous spectra at two heights show most spicules to have the same line-of-sight velocity at both. There may be an additional class of features, mostly rapidly moving, whose members have line-of-sight velocities that increase with height. These features comprise perhaps 10% of the total. Velocity changes occur simultaneously, to within 20 sec, at two heights separated by 1800 km, indicating velocities of propagation of hundreds of km/sec. The velocity field of individual features is often quite complicated; many spectral features are inclined to the direction of dispersion, implying that differential mass motions are present.
3. The existence of anomalously broad H and K profiles is real. Even with high dispersion and the best seeing, such profiles are not resolved into smaller features. The central reversal in K, H and Hα appears to remain unshifted when the wings are displaced in wavelength, indicating that the reversal is non-spicular.

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Coronal rotation during solar cycle 20     

G. D. Parker  R. T. Hansen  S. F. Hansen 《Solar physics》1982,80(1):185-198

Using K-coronameter observations made by the High Altitude Observatory at Haleakala and Mauna Loa, Hawaii during 1964–1976, we determine the apparent recurrence period of white-light solar coronal features as a function of latitude, height, and time. A technique based on maximum entropy spectral analysis is used to produce rotational period estimates from daily K-coronal brightness observations at 1.125R _S and 1.5R _S from disk center and at angular intervals of 5° around the Sun's limb. Our analysis reaffirms the existence of differential rotation in the corona and describes both its average behavior and its large year-to-year variations. On the average, there is less differential rotation at the greater height. After 1966–1967 we observe a general increase in coronal rotation rate which may relate to similar behavior reported for the equatorial photospheric Doppler rate. However, the coronal rate increase is significantly greater than the photospheric. If K-coronal features reflect the rotation at depth in the Sun, the long-term rate increase and the variable differential rotation may be evidence for dynamically important exchanges of energy and momentum in the upper convection zone.  相似文献