127 research outputs found
On the Fundamental Mass-Period Functions of Extrasolar Planets
Employing a catalog of 175 extrasolar planets (exoplanets) detected by the
Doppler-shift method, we constructed the independent and coupled mass-period
functions. It is the first time in this field that the selection effect is
considered in the coupled mass-period functions. Our results are consistent
with those in Tabachnik and Tremaine (2002) with the major differences that we
obtain a flatter mass function but a steeper period function. Moreover, our
coupled mass-period functions show that about 2.5 percent of stars would have a
planet with mass between Earth Mass and Neptune Mass, and about 3 percent of
stars would have a planet with mass between Neptune Mass and Jupiter Mass.Comment: Accepted by ApJ Supplement Series in Nov. 2009, Acknowledgment added
in Dec. 2009, a Reference-Based Catalog of Exoplanets can be obtained
electronically from Appendix A of the latex file or from the authors for
further studies
Spectra of High-Ionization Seyfert 1 Galaxies: Implications for the Narrow-Line Region
We present line profiles and profile parameters for the Narrow-Line Regions (NLRs) of six Seyfert 1 galaxies with high-ionization lines: MCG 8-11-11, Mrk 79, Mrk 704, Mrk 841, NGC 4151, and NGC 5548. The sample was chosen primarily with the goal of obtaining high-quality [Fe VII] lambda6087 and, when possible, [Fe X] lambda6374 profiles to determine if these lines are more likely formed in a physically distinct 'coronal line region' or are formed throughout the NLR along with lines of lower critical density (n(sub cr)) and/or Ionization Potential (IP). We discuss correlations of velocity shift and width with n(sub cr) and IP. In some objects, lines of high IP and/or n(sub cr) are systematically broader than those of low IP/n(sub cr). Of particular interest, however, are objects that show no correlations of line width with either IP or n(sub cr). In these objects, lines of high and low IP/n(sub cr), are remarkably similar, which is difficult to reconcile with the classical picture of the NLR, in which lines of high and low IP/n(sub cr) are formed in physically distinct regions. We argue for similar spatial extents for the flux in lines with similar profiles. Here, as well as in a modeling-oriented companion paper, we develop further an idea suggested by Moore & Cohen that objects that do and do not show line width correlations with IP/n(sub cr) can both be explained in terms of a single NLR model with only a small difference in the cloud column density distinguishing the two types of object. Overall, our objects do not show correlations between the Full Width at Half-Maximum (FWHM) and IP and/or n(sub cr). The width must be defined by a parameter that is sensitive to extended profile wings in order for the correlations to result. We present models in which FWHM correlations with IP and/or n(sub cr) result only after simulating the lower spectral resolution used in previous observational studies. The models that simulate the higher spectral resolution of our observational study produce line width correlations only if the width is defined by a parameter that is more sensitive to extended profile wings than is the FWHM. Our sample of six objects is in effect augmented by incorporating the larger sample (16 objects) of Veilleux into some of our discussion. This paper focuses on new interpretations of NLR emission-line spectra and line profiles that stem directly from the observations. Paper 2 focuses on modeling and complements this paper by illustrating explicitly the effects that spatial variations in electron density, ionization parameter, and column density have on model profiles. By comparing model profiles with the observed profiles presented here, as well as with those presented by Veilleux, Paper 2 yields insight into how the electron density, ionization parameter, and column density likely vary throughout the NLR
Planetary mass function and planetary systems
With planets orbiting stars, a planetary mass function should not be seen as
a low-mass extension of the stellar mass function, but a proper formalism needs
to take care of the fact that the statistical properties of planet populations
are linked to the properties of their respective host stars. This can be
accounted for by describing planet populations by means of a differential
planetary mass-radius-orbit function, which together with the fraction of stars
with given properties that are orbited by planets and the stellar mass function
allows to derive all statistics for any considered sample. These fundamental
functions provide a framework for comparing statistics that result from
different observing techniques and campaigns which all have their very specific
selection procedures and detection efficiencies. Moreover, recent results both
from gravitational microlensing campaigns and radial-velocity surveys of stars
indicate that planets tend to cluster in systems rather than being the lonely
child of their respective parent star. While planetary multiplicity in an
observed system becomes obvious with the detection of several planets, its
quantitative assessment however comes with the challenge to exclude the
presence of further planets. Current exoplanet samples begin to give us first
hints at the population statistics, whereas pictures of planet parameter space
in its full complexity call for samples that are 2-4 orders of magnitude
larger. In order to derive meaningful statistics however, planet detection
campaigns need to be designed in such a way that well-defined
fully-deterministic target selection, monitoring, and detection criteria are
applied. The probabilistic nature of gravitational microlensing makes this
technique an illustrative example of all the encountered challenges and
uncertainties.Comment: 7 pages, MNRAS accepte
A Blind Search for Magnetospheric Emissions from Planetary Companions to Nearby Solar-type Stars
This paper reports a blind search for magnetospheric emissions from planets
around nearby stars. Young stars are likely to have much stronger stellar winds
than the Sun, and because planetary magnetospheric emissions are powered by
stellar winds, stronger stellar winds may enhance the radio luminosity of any
orbiting planets. Using various stellar catalogs, we selected nearby stars (<~
30 pc) with relatively young age estimates (< 3 Gyr). We constructed different
samples from the stellar catalogs, finding between 100 and several hundred
stars. We stacked images from the 74-MHz (4-m wavelength) VLA Low-frequency Sky
Survey (VLSS), obtaining 3\sigma limits on planetary emission in the stacked
images of between 10 and 33 mJy. These flux density limits correspond to
average planetary luminosities less than 5--10 x 10^{23} erg/s. Using recent
models for the scaling of stellar wind velocity, density, and magnetic field
with stellar age, we estimate scaling factors for the strength of stellar
winds, relative to the Sun, in our samples. The typical kinetic energy carried
by the stellar winds in our samples is 15--50 times larger than that of the
Sun, and the typical magnetic energy is 5--10 times larger. If we assume that
every star is orbited by a Jupiter-like planet with a luminosity larger than
that of the Jovian decametric radiation by the above factors, our limits on
planetary luminosities from the stacking analysis are likely to be a factor of
10--100 above what would be required to detect the planets in a statistical
sense. Similar statistical analyses with observations by future instruments,
such as the Low Frequency Array (LOFAR) and the Long Wavelength Array (LWA),
offer the promise of improvements by factors of 10--100.Comment: 11 pages; AASTeX; accepted for publication in A
Evaluation of a multifaceted "Resident-as-Teacher" educational intervention to improve morning report
BACKGROUND: Resident-led morning report is an integral part of most residency programs and is ranked among the most valuable of educational experiences. The objectives of this study were to evaluate the effect of a resident-as-teacher educational intervention on the educational and teaching experience of morning report. METHODS: All senior internal medicine residents were invited to participate in this study as teaching participants. All internal medicine residents and clerks were invited to participate as audience participants. The educational intervention included reading material, a small group session and feedback after teaching sessions. The educational and teaching experiences were rated prior to and three months after the intervention using questionnaires. RESULTS: Forty-six audience participants and 18 teaching participants completed the questionnaires. The degree to which morning report met the educational needs of the audience was higher after the educational intervention (effect size, d = 0.26, p = 0.01). The perceptions of the audience were that delivery had improved and that the sessions were less intimidating and more interactive. The perception of the teaching participants was that delivery was less stressful, but this group now reported greater difficulty in engaging the audience and less confidence in their medical knowledge. CONCLUSION: Following the educational intervention the audience's perception was that the educational experience had improved although there were mixed results for the teaching experience. When evaluating such interventions it is important to evaluate the impact on both the educational and teaching experiences as results may differ
Biosignatures from Earth-Like Planets Around M Dwarfs
Coupled one-dimensional photochemical-climate calculations have been
performed for hypothetical Earth-like planets around M dwarfs. Visible,
near-infrared and thermal-infrared synthetic spectra of these planets were
generated to determine which biosignature gases might be observed by a future,
space-based telescope. Our star sample included two observed active M dwarfs,
AD Leo and GJ 643, and three quiescent model stars. The spectral distribution
of these stars in the ultraviolet generates a different photochemistry on these
planets. As a result, the biogenic gases CH4, N2O, and CH3Cl have substantially
longer lifetimes and higher mixing ratios than on Earth, making them
potentially observable by space-based telescopes. On the active M-star planets,
an ozone layer similar to Earth's was developed that resulted in a
spectroscopic signature comparable to the terrestrial one. The simultaneous
detection of O2 (or O3) and a reduced gas in a planet's atmosphere has been
suggested as strong evidence for life. Planets circling M stars may be good
locations to search for such evidence.Comment: 34 pages, 10 figures, Astrobiology, in pres
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