The Man in the Background: The Search for Maecenas

Antichthon ◽  
2020 ◽  
Vol 54 ◽  
pp. 54-79
Author(s):  
Ronald T. Ridley

AbstractSince the late sixteenth century parts of the ‘imperial frieze’ of the Ara Pacis have been known. The most striking figure in the background of the southern frieze is that long thought to be a portrait of Maecenas, the Etruscan prince and literary patron of the Augustan era. This article attempts three things: to discover 1.Where and how this identification originated,2.What evidence there now is for that identification, and3.What alternative identifications can be offered.The bibliography is substantial, the trail is complicated and highly paradoxical, and fantasy has often played a large role. The ‘evidence’ in play for centuries has sometimes evaporated into thin air. The identities proposed are, in fact, numerous. Not of least interest is the hidden or mistaken identity, in turn, of crucial modern scholars. A method is proposed at last for evaluating the identifications of this background portrait, including obvious comparison with other background figures. This analysis emphasizes how much is still not known about the most famous piece of Augustan art. An attempt is nevertheless made in the last analysis, to support what can be offered, in the light of current understanding, as the most plausible identification.

Author(s):  
Tomura ◽  
Okano ◽  
Hara

The recent advancement in scientific instrumentation has been phenomenal. This is particularity true in the electron probe microanalyzer field. This paper describes the improvements made in the Hitachi Model XMA-5 Electron Probe Microanalyzer to achieve high performance.1.X-ray spectroscopy1-1.It is now possible to analyze a wide variety of elements including ultra light elements in minute concentrations with the advent of an increasing number of dispersing elements and high detectability.1-2.A linear crystal drive and direct wavelength read-out (with respect to the crystal) is employed in the spectrometer to assure simultaneous analyses of up to three elements by using three of the six crystals provided. For correction of absorbed X-rays and fluorescence excitation and with due consideration of the angular distribution of the characteristic X-rays, an X-ray take off angle of 38° (electron probe is incident vertically on the specimen surface) was adopted.


1996 ◽  
Vol 173 ◽  
pp. 349-350 ◽  
Author(s):  
R.W. Porcas ◽  
A.R. Patnaik ◽  
T.W.B. Muxlow ◽  
M.A. Garrett ◽  
D. Walsh

We present new arcsecond-scale radio images of the gravitational lens system 0957+561 A, B. Observations at 1.6GHz were made in 1991 October with the VLA in A/B configuration with a resolution of 1.5 arcsec (Fig. 1, left). The lowest contour is 0.37 mJy/beam. In addition to the compact A and B image components, and the familiar NE/SW radio double-lobe structure surrounding image A, this map shows two interesting new features: (a)a long, thin feature extending south and west from the NE lobe, some 10 arcsec in extent, confirming the detection by Avruch et al. (1994). It is reminiscent of the ‘arc’ features seen in optical images of lensing clusters, and hopefully can be used to constrain models of the cluster mass distribution. (For the superstitious, one can note that the position angle of the arc, 17°, is identical to that of the VLBI jet in image B, a few arcseconds to the west.)(b)a low-level extension of the B image in the NW direction. We are not aware that this has been seen before. A possible interpretation of this feature is a continuation of the jet emission seen in VLBI images of B, whose counterpart in A is seen in higher resolution maps. The change of position angle between the VLBI and arcsec-scale jets would indeed have opposite parities in the A and B images.


1928 ◽  
Vol 74 (304) ◽  
pp. 35-49 ◽  
Author(s):  
R. Langdon-Down

The Royal Commission on Lunacy and Mental Disorder was set up in July, 1924, to inquire into a matter of urgent public importance, that is to say: (1)The existing law and administrative machinery in England and Wales in connection with the certification, detention and care of persons who are, or who are alleged to be, of unsound mind.(2)The extent to which provision is or should be made in England and Wales for the treatment without certification of persons suffering from mental disorder and to make recom mendations.


Radiocarbon ◽  
1967 ◽  
Vol 9 ◽  
pp. 1-14 ◽  
Author(s):  
C. Vance Haynes ◽  
Donald C. Grey ◽  
Paul E. Damon ◽  
Richmond Bennett

The C14 measurements reported here were made in this laboratory between November 15, 1965 and June 15, 1966. Sample descriptions are classified as follows: I.Geochemical SamplesII.Geologic-Paleoclimatic SamplesIII.Early Man-Alluvial Stratigraphy SamplesIV.Archaeologic Samples


Radiocarbon ◽  
1966 ◽  
Vol 8 ◽  
pp. 1-21 ◽  
Author(s):  
C. Vance Haynes ◽  
Paul E. Damon ◽  
Donald C. Grey

The C14 measurements reported here were made in this laboratory between November 1, 1963 and November 15, 1965. Sample descriptions are classified as follows: I.Geochemical SamplesII.Geologic-Paleoclimatic SamplesIII.Early Man-Alluvial Stratigraphy SamplesIV.Archaeologic Samples


Author(s):  
J. Newton Friend ◽  
John P. Allchin

Many attempts have been made to discover the causes of the various colours displayed by minerals. If we except fluorescence and allied phenomena, the diiteren~ theories advanced may in general be grouped under one or other of the following classes:(1)Colour may be due to an intrinsic property of atoms, ions, or molecules. Examples are copper atoms, chromate ions, and ferric oxide molecules.(2)Colour is sometimes attributed to structural causes. The blue tints of certain halites have been explained in this way; but a fresh suggestion is made in this communication.(3)A pigmentary impurity may cause the observed colour. The colour of the ruby is believed to be caused by the presence of a red chromic oxide. The blue tint of a Yorkshire aragonite is shown later to be due to a copper salt.(4)Some minerals show plays of colours due to interference and/or grating effects. Labradorite and opal are cases in point. Into this group also fall minerals like bomite which become iridescent from tarnish.


1958 ◽  
Vol 5 ◽  
pp. 69-73 ◽  
Author(s):  
J. H. Oort

A comparison of the Galactic System with other stellar systems might be based on: (a)the regular aspect (the population 11);(b)what we might call the semi-chaotic aspect, presented by the gas and the other population 1 objects;(c)the spherical corona of continuous radio-emission.As far as (a) is concerned we are not yet in a position to say very much. The only type of objects of extreme population 11 that we have recognized with certainty in the Galactic System as well as in other comparable systems are the globular clusters. They are very incompletely known in the Galaxy, perhaps somewhat more completely in the Andromeda nebula, but few systematic studies have been made in other systems. So far as we can tell, the Andromeda nebula and the Galactic System are comparable in the number and general distribution of globular clusters.


Radiocarbon ◽  
1963 ◽  
Vol 5 ◽  
pp. 283-301 ◽  
Author(s):  
Paul E. Damon ◽  
Austin Long ◽  
Joel J. Sigalove

C14 measurements reported here were made in this laboratory between December 1, 1961 and October 1, 1962. Sample descriptions are classified as follows: I.Tree-ring dated samples.II.Modern shells from Santa Barbara County, California.III.Archaeologic samples.IV.Palynologic samples.V.Geologic samples.VI.C14 content of caliche.VII.Water samples.VIII.Modern organic sample.


1994 ◽  
Vol 144 ◽  
pp. 431-434
Author(s):  
M. Minarovjech ◽  
M. Rybanský

AbstractThis paper deals with a possibility to use the ground-based method of observation in order to solve basic problems connected with the solar corona research. Namely:1.heating of the solar corona2.course of the global cycle in the corona3.rotation of the solar corona and development of active regions.There is stressed a possibility of high-time resolution of the coronal line photometer at Lomnický Peak coronal station, and use of the latter to obtain crucial observations.


1994 ◽  
Vol 144 ◽  
pp. 279-282
Author(s):  
A. Antalová

AbstractThe occurrence of LDE-type flares in the last three cycles has been investigated. The Fourier analysis spectrum was calculated for the time series of the LDE-type flare occurrence during the 20-th, the 21-st and the rising part of the 22-nd cycle. LDE-type flares (Long Duration Events in SXR) are associated with the interplanetary protons (SEP and STIP as well), energized coronal archs and radio type IV emission. Generally, in all the cycles considered, LDE-type flares mainly originated during a 6-year interval of the respective cycle (2 years before and 4 years after the sunspot cycle maximum). The following significant periodicities were found:• in the 20-th cycle: 1.4, 2.1, 2.9, 4.0, 10.7 and 54.2 of month,• in the 21-st cycle: 1.2, 1.6, 2.8, 4.9, 7.8 and 44.5 of month,• in the 22-nd cycle, till March 1992: 1.4, 1.8, 2.4, 7.2, 8.7, 11.8 and 29.1 of month,• in all interval (1969-1992):a)the longer periodicities: 232.1, 121.1 (the dominant at 10.1 of year), 80.7, 61.9 and 25.6 of month,b)the shorter periodicities: 4.7, 5.0, 6.8, 7.9, 9.1, 15.8 and 20.4 of month.Fourier analysis of the LDE-type flare index (FI) yields significant peaks at 2.3 - 2.9 months and 4.2 - 4.9 months. These short periodicities correspond remarkably in the all three last solar cycles. The larger periodicities are different in respective cycles.


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