Boron Abundance in the PopII HD 76932

1988 ◽  
Vol 132 ◽  
pp. 511-514
Author(s):  
P. Molaro
Keyword(s):  
High Resolution ◽  
Preliminary Analysis ◽  
The Other ◽  
Light Elements ◽  
Simultaneous Presence ◽  
The Past ◽  
Upper Limits ◽  
Cool Stars ◽  
The Galaxy ◽  
The Continuum

Aware of the importance of B observations in cool stars we have attempted to search for BI 2496 lines in high resolution IUE spectra of HD 76932, with [Fe/H]=−1.1, and HD 216385, with [Fe/H]=−0.6. Line blending and the impossibility of establishing the continuum level are the major obstacles in such an investigation. Molaro (1987) showed that, in the case of extremely metal-deficient stars, the consequent line-blocking reduction allows us to derive significant upper limits for the B abundance. In HD 140283, [Fe/H]=−3.0, Molaro (1987) derived [B/H]< 2 ×10−11. In HD 76932 a preliminary analysis gives a B abundance of [B/H]< 2 ×10−10, i.e. less than the present “cosmic” value. On the other hand no useful limits can be placed for HD 216385. The presence of an unidentified line, not resolved with IUE, prevents B analysis in cool stars with similar or greater metallicity. Better data with higher spectral resolution and greater photometric accuracy are required to confirm these results. The simultaneous presence of Li in the atmospheres of these stars rules out stellar depletion for B, providing evidence that the B abundance in the Galaxy was lower in the past than it is today. These observations also imply that spallation proccesses were not able to produce significant quantities of B, or other light elements at the beginning of the Galaxy. In particular, spallation processes cannot be adduced as a possible source for the Li observed in the Pop II stars.

scholarly journals Massive Star Formation in W49

1987 ◽  
Vol 115 ◽  
pp. 143-145
Author(s):  
J. Dreher ◽  
S. Vogel ◽  
S. Terebey ◽  
W. J. Welch
Keyword(s):  
Star Formation ◽  
High Resolution ◽  
Massive Star ◽  
Hii Regions ◽  
Molecular Line ◽  
The Galaxy ◽  
Molecular Lines ◽  
H Ii Region ◽  
Scale Structures ◽  
The Continuum

W49 is the most luminous H II region complex in the galaxy. VLA maps in the continuum reveal a complex of more than two dozen compact HII regions, including a ring-like distribution of a dozen such regions within a volume of 1 pc. In addition to the VLA maps, we have obtained high resolution maps in this field with the Hat Creek Millimeter Interferometer in the following molecular lines: HCO+(1-0), H13CO+(1-0), SiO(v = 0, J = 2-1), SiO(v = 1, J = 2-1), H13CN(1-0), HC15N(1-0), SO2 [8(3,5)-9(2,8)], SO2[8(1,7)-8(0,8)], SO[2(2)-1(1)], and CH3CH2CN[10(1,10)-9(1,9)], all near 3 mm wavelengh. These maps will be discussed. The HCO+distribution corresponds to the larger scale structures observed in the continuum maps. In contrast the SO and SiO sources are quite compact. Using the detailed molecular line results obtained in the ORION/KL region as a guide, we are able to identify these latter sources as regions in which the star formation is at an earlier stage, regions where there are outflows.

scholarly journals The 12C/13C Ratio in Unevolved Cool Stars

1988 ◽  
Vol 132 ◽  
pp. 589-592
Author(s):  
Y. Chmielewski ◽  
D. L. Lambert
Keyword(s):  
High Resolution ◽  
Preliminary Analysis ◽  
Isotope Ratio ◽  
Signal To Noise Ratio ◽  
Carbon Isotope Ratio ◽  
High Signal ◽  
Reasonable Accuracy ◽  
Signal To Noise ◽  
Dwarf Stars ◽  
Cool Stars

We show that the carbon isotope ratio 12C/13C in the atmosphere of dwarf stars can be determined with reasonable accuracy from high resolution, high signal-to-noise ratio observations of the CH G-band in their spectra. Lines suitable for this purpose are selected from consideration of the solar case, for which 12C/13C = 89 is derived. A preliminary analysis of these features in the spectra of μ Her, δ Eri and τ Cet yields 12C/13C values of 84, 80 and 150 respectively.

Gatekeepers of (Non-)Knowledge: Aleksei Balabanov’s Morphine (2008)

2016 ◽  
Author(s):  
Vlad Strukov
Keyword(s):  
Cultural Memory ◽  
The Self ◽  
The Other ◽  
Cultural Discourse ◽  
The Past ◽  
The Future ◽  
The Subject ◽  
Self Organisation ◽  
The Continuum

Balabanov’s Morphine is concerned with cultural memory conceived as a continuum; not as identity but rather subjectivity in construction. The concepts relates to Badiou’s study of subjectivity. It determines existence in a world where the horizon of knowledge is always disappearing and is never available to us in its integrity whereby the subject is barred from the infinite. Different directions and speeds of movement generate the transcendental subject in that the subject is in relation to the variations of the lived. One of such states implies a continuum, or becoming without determination, whilst the other, refers to the imperative to construct knowledge out of the elements of the continuum. Such assemblages, rituals and rites allow the subject to access the ‘beyond’, a different realm, where the elements of the past are positioned towards the future. The transcendence of the subject is coded as an unstoppable flow of imagery—a hallucination—divided into sequences by reiterations and references to the cultural discourse: an introspective vision produces not self-organisation but self-destruction as the subject becomes aware of its own infiniteness. I showcase how Balabanov’s Morphine captures the brutality of such openings and the self-annihilating impact of nothingness.

scholarly journals HESS Opinions: The complementary merits of competing modelling philosophies in hydrology

2017 ◽  
Vol 21 (8) ◽  
pp. 3953-3973 ◽  
Author(s):  
Markus Hrachowitz ◽  
Martyn P. Clark
Keyword(s):  
High Resolution ◽  
Extreme Case ◽  
The Other ◽  
Small Scale ◽  
Hydrological Models ◽  
Hydrological Response ◽  
Linear Transfer Function ◽  
Modelling Strategies ◽  
Process Based Models ◽  
The Continuum

Abstract. In hydrology, two somewhat competing philosophies form the basis of most process-based models. At one endpoint of this continuum are detailed, high-resolution descriptions of small-scale processes that are numerically integrated to larger scales (e.g. catchments). At the other endpoint of the continuum are spatially lumped representations of the system that express the hydrological response via, in the extreme case, a single linear transfer function. Many other models, developed starting from these two contrasting endpoints, plot along this continuum with different degrees of spatial resolutions and process complexities. A better understanding of the respective basis as well as the respective shortcomings of different modelling philosophies has the potential to improve our models. In this paper we analyse several frequently communicated beliefs and assumptions to identify, discuss and emphasize the functional similarity of the seemingly competing modelling philosophies. We argue that deficiencies in model applications largely do not depend on the modelling philosophy, although some models may be more suitable for specific applications than others and vice versa, but rather on the way a model is implemented. Based on the premises that any model can be implemented at any desired degree of detail and that any type of model remains to some degree conceptual, we argue that a convergence of modelling strategies may hold some value for advancing the development of hydrological models.

scholarly journals Distribution and motions of HI in M31

1985 ◽  
Vol 106 ◽  
pp. 437-442
Author(s):  
E. Brinks ◽  
W. B. Burton
Keyword(s):  
High Resolution ◽  
Atomic Hydrogen ◽  
Line Of Sight ◽  
Complete Model ◽  
Previous Survey ◽  
The Past ◽  
The Galaxy ◽  
The One

It has become clear in the past few years that the distribution and kinematics of HI in M31 is far from simple. The new high-resolution survey made with the Westerbork SRT in the 21-cm line of atomic hydrogen by Brinks and Shane (1983) shows this dramatically. Along almost any line of sight through M31 two separate velocity systems are sampled. Based on a previous survey Shane (1978) and later Bajaja and Shane (1982) proposed that the extra component is due to warping of the plane of the galaxy into the direction of and crossing the line-of-sight. Roberts et al. (1978) and Whitehurst et al. (1978) emphasized that the observed profile structure ruled out confinement of the gas to a thin plane. Unwin (1983) reached a similar conclusion on the basis of his survey. The most complete model produced up until now which accounts for the two velocity systems is the one by Henderson (1979), based on the 100-m Effelsberg survey of M31 by Cram et al. (1980)

Ann Schein

2017 ◽  
Author(s):  
Cecelia Hopkins Porter
Keyword(s):  
The Other ◽  
Western Society ◽  
Career Centers ◽  
The Past ◽  
American Artist ◽  
Women In Music ◽  
The Continuum

This chapter discusses Ann Schein (November 10, 1939–) in contrast to the other women previously mentioned. She is here as someone at the living edge of the continuum in Western society, a non-European whose career centers on public concert performance. Thus the bulk of the research in this chapter is conducted in interviews the author has made with Schein between 2005 and 2009. A present-day artist, Schein can speak about herself firsthand, adding a further dimension to our understanding of her and casting light on earlier women in music in a way not possible with those of the past. The present examination of Schein's life, both private and professional, offers a type of evidence that can shed unique light not only on the past, but also on the present by way of an American artist still intensely active.

scholarly journals The ultraviolet spectrum of AG Draconis

1982 ◽  
Vol 70 ◽  
pp. 183-184
Author(s):  
A. Altamore ◽  
G.B. Baratta ◽  
A. Cassatella ◽  
A. Giangrande ◽  
D. Ponz ◽  
...  
Keyword(s):  
High Resolution ◽  
Light Curve ◽  
Ultraviolet Spectrum ◽  
The Other ◽  
Emission Lines ◽  
Symbiotic Stars ◽  
Low Resolution ◽  
Uv Spectrum ◽  
O 69 ◽  
The Continuum

The high resolution ultraviolet spectrum of AG Dra was observed with IUE in April and August 1981 at phases 0.50 and O.69 according to the Meinunger (1979, Inf. Bull. Var. Stars No.1611) U-light curve. The UV spectrum of the star appears rather different from that of the other classical symbiotic stars. The low resolution IUE spectrum of AG Dra shown in figure 1. The continuum is rather strong with respect to the emission lines and detectable at high resolution. Many intense interstellar lines are present, in spite of the low reddening of the star (E(B-V)=0.06, according to the depth of the 2200A interstellar band).

Automated Spectrophotometry

1971 ◽  
Vol 11 ◽  
pp. 179-182
Author(s):  
G. I. Thompson
Keyword(s):  
Spatial Frequency ◽  
The Other ◽  
Stellar Spectrum ◽  
Low Frequencies ◽  
High Frequencies ◽  
The Past ◽  
Other Hand ◽  
Spatial Frequencies ◽  
Special Cases ◽  
The Continuum

Starting from a digitized and calibrated stellar spectrum—what can we most usefully do with it?Traditionally a spectrum consists of two parts, a continuum and some lines. These have been variously defined in the past, so perhaps another definition may be allowed. Over large ranges the two components can be distinguished quite sharply in the spatial frequency plane. The continuum contains only low frequencies, whereas in the line the information is contained in the high frequencies. In the word “continuum” is included the instrumental absorption functions, emulsion sensitivity, wide interstellar and atmospheric bands, and even the wide wings of very strong lines. From the word “lines”, on the other hand, the strongest lines are excluded; these may contain intermediate spatial frequencies in their core regions. They are relatively infrequent and so may be treated as special cases.

The Role of Structural Organisation and Myth in Javanese Historiography

1964 ◽  
Vol 24 (1) ◽  
pp. 91-99 ◽  
Author(s):  
Anthony H. Johns
Keyword(s):  
Cultural History ◽  
The Other ◽  
Indian Culture ◽  
Historical Process ◽  
Structural Organisation ◽  
Dead End ◽  
The Galaxy ◽  
The One ◽  
The Continuum

The galaxy of non-indigenous elements confronting the student of Indonesian cultural history has often obscured the fact that, in order to elucidate a valid picture of their role and significance, these elements need to be studied in their own terms, in relation to their own environment and at specific synchronic levels, such levels being but points on the continuum of the historical process. Thus to consider Javanese culture exclusively as a linear (and corrupt) descendant of Indian culture on the one hand, or as perpetually conditioned by a hypothetical indigenous ur-society in the manner of Rassers on the other, leads to a dead end, and has stultified much otherwise useful and impressive research.

scholarly journals High Resolution Interferometry of Cool Stars

1974 ◽  
Vol 3 ◽  
pp. 237-254
Author(s):  
D. L. Lambert
Keyword(s):  
Infrared Spectroscopy ◽  
High Resolution ◽  
Lower Limit ◽  
Preliminary Analysis ◽  
Cool Stars ◽  
M Stars ◽  
Vibration Rotation

AbstractThis paper reviews results obtained in a program of high resolution infrared spectroscopy of K and M giants. The reported results include (i) a preliminary analysis of the C, N and O abundances for α Ori, (ii) determinations of the 12C/13C and 16O/18O ratios for α Ori (12C/13C ~ 6 and 16O/18 ~ 500), (iii) the derivation of a lower limit, 16O/18O≳ 300, for the 160/18O ratio in α Boo, (iv) a discussion of observations of the SiO first-overtone vibration-rotation bands in M stars, and (v) a search for the fundamental quadrupole vibration-rotation lines of H2.

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