ChemInform Abstract: INTERACTION OF A PHENYLPYRAZOLIDINE URETHANE WITH MEERWEIN′S SALT

Barcza, Sándor; Eberle, Marcel K.; Engstrom, Nancy.; KAHLE, G. G.

doi:10.1002/chin.197630179

Cited by 2 publications

(3 citation statements)

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“…Even without recent improvements in stellar modeling and various means to determine the temperature of a star such as with widths of metal lines, the temperature of RR Lyrae stars have previously been determined down to 20 K with only K and V band photometry (see (Cacciari et al 1992) for further references). Barcza (2010); Barcza & Benkő (2012) has formulated a new way to directly model the size mass, radius and temperature of the star by exploiting multiple bands-No spectral information. The authors could determine the temperature to within 20 K and limit the mass to better than 4 percent.…”

Section: Feasibilitymentioning

confidence: 99%

“…The authors could determine the temperature to within 20 K and limit the mass to better than 4 percent. We emphasis that the conclusions drawn by Barcza (2010); Barcza & Benkő (2012) were made without the benefit of deep infrared band coverage (H, J, and K) and without the use of any spectral information. In terms of surface velocity, we note that with the addition of spectral information, we can measure the expansion of a star down to a fraction of a km/s.…”

Section: Feasibilitymentioning

confidence: 99%

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Plan β: core or cusp?

Richardson

Spolyar

Lehnert

2014

Monthly Notices of the Royal Astronomical Society

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The inner profile of Dark Matter (DM) halos remains one of the central problems in small-scale cosmology. At present, the problem can not be resolved in dwarf spheroidal galaxies due to a degeneracy between the DM profile and the velocity anisotropy β of the stellar population. We discuss a method which can break the degeneracy by exploiting 3D positions and 1D line-of-sight (LOS) velocities. With the full 3D spatial information, we can determine precisely what fraction of each stars LOS motion is in the radial and tangential direction. This enables us to infer the anisotropy parameter β directly from the data. The method is particularly effective if the galaxy is highly anisotropic. Finally, we argue that such a test could be applied to Sagittarius and potentially other dwarfs with RR Lyrae providing the necessary depth information.

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Section: Feasibilitymentioning

confidence: 99%

Section: Feasibilitymentioning

confidence: 99%

Plan β: core or cusp?

Richardson

Spolyar

Lehnert

2014

Monthly Notices of the Royal Astronomical Society

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“…The first and second parts of this series of papers (Barcza 2010 andBenkő 2012, hereafter Papers I and II) described a new method to determine the fundamental parameters of spherically pulsating stars with large amplitude, e.g. of RR Lyrae (hereafter RR) stars.…”

Section: Introductionmentioning

confidence: 99%

Fundamental parameters of RR Lyrae stars from multicolour photometry and Kurucz atmospheric models – III. SW And, DH Peg, CU Com and DY Peg

Barcza

Benkő

2014

Monthly Notices of the Royal Astronomical Society

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We report the most comprehensive UBV(RI) C observations of the bright, radially pulsating field stars SW And, DH Peg, CU Com, DY Peg. Long term variation has been found in the ultraviolet colour curves of SW And and DH Peg. We apply our photometric-hydrodynamic method to determine the fundamental parameters of these stars: metallicity, reddening, distance, mass, radius, equilibrium luminosity and effective temperature. Our method works well for SW And, CU Com and DY Peg. A very small mass 0.26 ± 0.04 M ⊙ of SW And has been found. The fundamental parameters of CU Com are those of a normal double-mode RR Lyrae (RRd) star. DY Peg has been found to have paradoxical astrophysical parameters: the metallicity, mass and period are characteristic for a high-amplitude δ Sct star while the luminosity and radius place it in the group of RR Lyrae stars. DH Peg has been found to be peculiar: the definite instability in the colour curves towards ultraviolet, the dynamical variability of the atmosphere during the shocked phases suggests that the main assumptions of our photometric-hydrodynamic method, the quasi-static atmosphere approximation (QSAA) and the exclusive excitation of radial modes are probably not satisfied in this star. The fundamental parameters of all stars studied in this series of papers are summarised in tabular and graphical form.

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ChemInform Abstract: INTERACTION OF A PHENYLPYRAZOLIDINE URETHANE WITH MEERWEIN′S SALT

Abstract: Phenyl‐pyrazolidin (Ia) wird zu (Ib) carbäthoxyliert und dann mit Triäthyloxoniumsalz zum Salz (II) substituiert, aus dem mit Äthylat das Spaltprodukt (IIIa) erhalten wird.

Cited by 2 publications

References 1 publication

Plan β: core or cusp?

Plan β: core or cusp?

Fundamental parameters of RR Lyrae stars from multicolour photometry and Kurucz atmospheric models – III. SW And, DH Peg, CU Com and DY Peg

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