1,362 research outputs found
A heavy Higgs boson from flavor and electroweak symmetry breaking unification
We present a unified picture of flavor and electroweak symmetry breaking
based on a nonlinear sigma model spontaneously broken at the TeV scale. Flavor
and Higgs bosons arise as pseudo-Goldstone modes. Explicit collective symmetry
breaking yields stable vacuum expectation values and masses protected at one
loop by the little-Higgs mechanism. The coupling to the fermions generates
well-definite mass textures--according to a U(1) global flavor symmetry--that
correctly reproduce the mass hierarchies and mixings of quarks and leptons. The
model is more constrained than usual little-Higgs models because of bounds on
weak and flavor physics. The main experimental signatures testable at the LHC
are a rather large mass m_{h^0} = 317\pm 80 GeV for the (lightest) Higgs boson
and a characteristic spectrum of new bosons and fermions at the TeV scale.Comment: 5 page
Photometric Properties of Kiso Ultraviolet-Excess Galaxies in the Lynx-Ursa Major Region
We have performed a systematic study of several regions in the sky where the
number of galaxies exhibiting star formation (SF) activity is greater than
average. We used Kiso ultraviolet-excess galaxies (KUGs) as our SF-enhanced
sample. By statistically comparing the KUG and non-KUG distributions, we
discovered four KUG-rich regions with a size of . One of these regions corresponds spatially to a filament of length
Mpc in the Lynx-Ursa Major region (). We call this ``the Lynx-Ursa
Major (LUM) filament''. We obtained surface photometry of 11 of
the KUGs in the LUM filament and used these to investigate the integrated
colors, distribution of SF regions, morphologies, and local environments. We
found that these KUGs consist of distorted spiral galaxies and compact galaxies
with blue colors. Their star formation occurs in the entire disk, and is not
confined to just the central regions. The colors of the SF regions imply that
active star formation in the spiral galaxies occurred yr ago,
while that of the compact objects occurred yr ago. Though the
photometric characteristics of these KUGs are similar to those of interacting
galaxies or mergers, most of these KUGs do not show direct evidence of merger
processes.Comment: 39 pages LaTeX, using aasms4.sty, 20 figures, ApJS accepted. The
Title of the previous one was truncated by the author's mistake, and is
corrected. Main body of the paper is unchange
KIC 4150611: a rare multi-eclipsing quintuple with a hybrid pulsator
We present the results of our analysis of KIC 4150611 (HD 181469) - an
interesting, bright quintuple system that includes a hybrid
Sct/ Dor pulsator. Four periods of eclipses - 94.2, 8.65, 1.52 and 1.43
d - have been observed by the Kepler satellite, and three point sources (A, B,
and C) are seen in high angular resolution images.
From spectroscopic observations made with the HIDES spectrograph attached to
the 1.88-m telescope of the Okayama Astrophysical Observatory (OAO), for the
first time we calculated radial velocities (RVs) of the component B - a pair of
G-type stars - and combined them with Kepler photometry in order to obtain
absolute physical parameters of this pair. We also managed to directly measure
RVs of the pulsator, also for the first time. Additionally, we modelled the
light curves of the 1.52 and 1.43-day pairs, and measured their eclipse timing
variations (ETVs). We also performed relative astrometry and photometry of
three sources seen on the images taken with the NIRC2 camera of the Keck II
telescope. Finally, we compared our results with theoretical isochrones.
The brightest component Aa is the hybrid pulsator, transited every 94.2 days
by a pair of K/M-type stars (Ab1+Ab2), which themselves form a 1.52-day
eclipsing binary. The components Ba and Bb are late G-type stars, forming
another eclipsing pair with a 8.65 day period. Their masses and radii are
M, R for the
primary, and M, R
for the secondary. The remaining period of 1.43 days is possibly related to a
faint third star C, which itself is most likely a background object. The
system's properties are well-represented by a 35 Myr isochrone. There are also
hints of additional bodies in the system.Comment: 14 pages, 15 figures, 7 tables, to appear in A&A, abstract modified
in order to fit the arXiv limi
Dynamical Generation of CKM Mixings by Broken Horizontal Gauge Interactions
The fermion mass matrices are calculated in the framework of the dynamical
mass generation by the broken horizontal gauge interactions. The
non-proportional mass spectra between up- and down-sectors and CKM mixings are
obtained solely by radiative corrections due to the ordinary gauge
interactions.Comment: 20 pages + 1 uuencoded eps figure, PHYZZ
A high fibered power of a family of varieties of general type dominates a variety of general type
We prove the following theorem:
Fibered Power Theorem: Let X\rar B be a smooth family of positive
dimensional varieties of general type, with irreducible. Then there exists
an integer , a positive dimensional variety of general type , and a
dominant rational map X^n_B \das W_n.Comment: Latex2e (in latex 2.09 compatibility mode). To get a fun-free version
change the `FUN' variable to `n' on the second line (option dedicated to my
friend Yuri Tschinkel). Postscript file with color illustration available on
http://math.bu.edu/INDIVIDUAL/abrmovic/fibered.p
Photospheric Abundances of Volatile and Refractory Elements in Planet-Harboring Stars
By using the high-dispersion spectra of 14 bright planet-harboring stars
(along with 4 reference stars) observed with the new coude echelle spectrograph
at Okayama Astrophysical Observatory, we investigated the abundances of
volatile elements (C, N, O, S, Zn; low condensation temperature Tc) in order to
examine whether these show any significant difference compared to the
abundances of other refractory elements (Si, Ti, V, Fe, Co, Ni; high Tc) which
are known to be generally overabundant in those stars with planets, since a
Tc-dependence is expected if the cause of such a metal-richness is due to the
accretion of solid planetesimals onto the host star. We found, however, that
all elements we studied behave themselves quite similarly to Fe (i.e.,
[X/Fe]~0) even for the case of volatile elements, which may suggest that the
enhanced metallicity in those planet-bearing stars is not so much an acquired
character (by accretion of rocky material) as rather primordial.Comment: 22 pages, 8 figures, to appear in PAS
Semantics and Proof Theory of the Epsilon Calculus
The epsilon operator is a term-forming operator which replaces quantifiers in
ordinary predicate logic. The application of this undervalued formalism has
been hampered by the absence of well-behaved proof systems on the one hand, and
accessible presentations of its theory on the other. One significant early
result for the original axiomatic proof system for the epsilon-calculus is the
first epsilon theorem, for which a proof is sketched. The system itself is
discussed, also relative to possible semantic interpretations. The problems
facing the development of proof-theoretically well-behaved systems are
outlined.Comment: arXiv admin note: substantial text overlap with arXiv:1411.362
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