45,128 research outputs found
2002 Survey of Rhode Island Law: Legislation: Business Law: An Act Relating to Corporations, Associations and Partnerships - Limited Liability Partnerships and the Rhode Island Limited Liability Company Act
War And The Business Corporation
http://deepblue.lib.umich.edu/bitstream/2027.42/39811/3/wp427.pd
AEIOU: Supervocalics in Webster\u27s Third
FOUNDING FATHERS and WOMAN SUFFRAGISTS, get out your FOUNTAIN PENS-it\u27s time for another visit to the world of AEIOU. To do justice to my fascination with all things AEIOU, I recently introduced the term SUPERVOCALIC to refer to any item, be it word, phrase or proper noun, containing each of the five vowels once and only once, and no Y. The term is modeled on the existing word \u27univocalic\u27 which describes a word or phrase that contains only one vowel (potentially repeated, as in \u27Mississippi\u27 or Ellen DeGeneres\u27). It has the added appeal of being self-referential, that is to say \u27supervocalic\u27 it self supervocalic
Confronting the Neighbors: Community Impact Panels in the Realm of Restorative Justice and Punishment Theory
They might be giants: luminosity class, planet frequency, and planet-metallicity relation of the coolest Kepler target stars
We estimate the stellar parameters of late K and early M type Kepler target
stars. We obtain medium resolution visible spectra of 382 stars with Kp-J>2
(~K5 and later spectral type). We determine luminosity class by comparing the
strength of gravity-sensitive indices (CaH, K I, Ca II, and Na I) to their
strength in a sample of stars of known luminosity class. We find that giants
constitute 96+-% of the bright (Kp<14) Kepler target stars, and 7+-3% of dim
(Kp>14) stars, significantly higher than fractions based on the stellar
parameters quoted in the Kepler Input Catalog (KIC). The KIC effective
temperatures are systematically (110 +15 -35} K) higher than temperatures we
determine from fitting our spectra to PHOENIX stellar models. Through Monte
Carlo simulations of the Kepler exoplanet candidate population, we find a
planet occurrence of 0.36+-0.08 when giant stars are properly removed, somewhat
higher than when a KIC log(g)>4 criterion is used (0.27+-0.05). Lastly, we show
that there is no significant difference in g-r color (a probe of metallicity)
between late-type Kepler stars with transiting Earth-to-Neptune sized exoplanet
candidates and dwarf stars with no detected transits. We show that a previous
claimed offset between these two populations is most likely an artifact of
including a large number of misidentified giants.Comment: Accepted to Ap
CC Bootis: QSO, Not Variable Halo Giant
The poorly-studied, faint (18<m_pg<19.5) variable star CC Bootis has been
noted in the literature as a candidate for a halo red giant. It proves instead
to be a quasi-stellar object of redshift z=0.172, and is detected as an X-ray
source by ROSAT. In addition to its odd heritage, CC Boo exhibits unusually
high amplitude optical variability for an optically-selected QSO.Comment: 6 pages including 1 table and 2 figures; Accepted for publication in
Pub. Astr. Soc. Pacific, Vol 109, June 199
M Dwarf Metallicities and Giant Planet Occurrence: Ironing Out Uncertainties and Systematics
Comparisons between the planet populations around solar-type stars and those
orbiting M dwarfs shed light on the possible dependence of planet formation and
evolution on stellar mass. However, such analyses must control for other
factors, i.e. metallicity, a stellar parameter which strongly influences the
occurrence of gas giant planets. We obtained infrared spectra of 121 M dwarfs
stars monitored by the California Planet Search (CPS) and determined
metallicities with an accuracy of 0.08 dex. The mean and standard deviation of
the sample is -0.05 and 0.20 dex, respectively. We parameterized the
metallicity dependence of the occurrence of giant planets on orbits with period
less than 2 yr around solar-type stars and applied this to our M dwarf sample
to estimate the expected number of giant planets. The number of detected
planets (3) is lower than the predicted number (6.4) but the difference is not
very significant (12% probability of finding as many or fewer planets). The
three M dwarf planet hosts are not especially metal rich and the most likely
value of the power-law index relating planet occurrence to metallicity is 1.06
dex per dex for M dwarfs compared to 1.80 for solar-type stars; this
difference, however, is comparable to uncertainties. Giant planet occurrence
around both types of stars allows, but does not necessarily require, mass
dependence of dex per dex. The actual planet-mass-metallicity relation
may be complex and elucidating it will require larger surveys like those to be
conducted by ground-based infrared spectrographs and the Gaia space astrometry
mission.Comment: Accepted to The Astrophysical Journa
- âŠ