175 research outputs found
Comparing Special Education Teachers’ Personality Profile With Their Choice to Teach
Researchers have yet to examine the association of Holland personality profiles as it relates to special education teachers. In response to this need, we report the personality and vocational profiles (Holland Codes) of 134 special education teachers across a special education training program. The purpose of this paper is to summarize findings from the Self-Directed Search measure commonly used to assess the personality of participants in an occupation and suggest implications for participants’ choice in becoming a special education teacher. Our focus was on personality match with vocational choice to include participants’ demographic (e.g., gender, race/ethnicity, and geographical location) profile. Findings from the study reveal that while special educators’ overall personality profile is congruent with the Holland Codes associated with special education teachers, other features may explain participants’ choice to pursue a career as a special education teacher. Implications for teacher preparation programs and K-12 schools training are recommended based on the research findings
Revised Properties and Dynamical History for the HD 17156 System
From the thousands of known exoplanets, those that transit bright host stars
provide the greatest accessibility toward detailed system characterization. The
first known such planets were generally discovered using the radial velocity
technique, then later found to transit. HD 17156b is particularly notable among
these initial discoveries because it diverged from the typical hot Jupiter
population, occupying a 21.2 day eccentric () orbit, offering
preliminary insights into the evolution of planets in extreme orbits. Here we
present new data for this system, including ground and space-based photometry,
radial velocities, and speckle imaging, that further constrain the system
properties and stellar/planetary multiplicity. These data include photometry
from the Transiting Exoplanet Survey Satellite (TESS) that cover five transits
of the known planet. We show that the system does not harbor any additional
giant planets interior to 10 AU. The lack of stellar companions and the age of
the system indicate that the eccentricity of the known planet may have resulted
from a previous planet-planet scattering event. We provide the results from
dynamical simulations that suggest possible properties of an additional planet
that culminated in ejection from the system, leaving a legacy of the observed
high eccentricity for HD 17156b.Comment: 15 pages, 7 figures, accepted for publication in the Astronomical
Journa
Revised Architecture and Two New Super-Earths in the HD 134606 Planetary System
Multi-planet systems exhibit a diversity of architectures that diverge from
the solar system and contribute to the topic of exoplanet demographics. Radial
velocity (RV) surveys form a crucial component of exoplanet surveys, as their
long observational baselines allow searches for more distant planetary orbits.
This work provides a significantly revised architecture for the multi-planet
system HD 134606 using both HARPS and UCLES RVs. We confirm the presence of
previously reported planets b, c, and d with periods
, , and
days, and masses , , and
Earth masses respectively, with the planet d orbit significantly
revised to over double that originally reported. We report two newly detected
super-Earths, e and f, with periods and
days, and masses and
Earth masses, respectively. In addition, we identify a
linear trend in the RV time series, and the cause of this acceleration is
deemed to be a newly detected sub-stellar companion at large separation. HD
134606 now displays four low mass planets in a compact region near the star,
one gas giant further out in the Habitable Zone, an additional massive
companion in the outer regime, and a low mass M dwarf stellar companion at
large separation, making it an intriguing target for system formation/evolution
studies. The location of planet d in the Habitable Zone proves to be an
exciting candidate for future space-based direct imaging missions, whereas
continued RV observations of this system are recommended for understanding the
nature of the massive, long period companion.Comment: 23 pages, 10 figures, 4 tables, accepted for publication in the
Astronomical Journa
Revised Architecture and Two New Super-Earths in the HD 134606 Planetary System
© 2024. The Author(s). Published by the American Astronomical Society. This is an open access article distributed under the terms of the Creative Commons Attribution License (CC BY), https://creativecommons.org/licenses/by/4.0/Multiplanet systems exhibit a diversity of architectures that diverge from the solar system and contribute to the topic of exoplanet demographics. Radial velocity (RV) surveys form a crucial component of exoplanet surveys, as their long observational baselines allow for searches for more distant planetary orbits. This work provides a significantly revised architecture for the multiplanet system HD 134606 using both HARPS and UCLES RVs. We confirm the presence of previously reported planets b, c, and d with periods of 12.0897 − 0.0018 + 0.0019 , 58.947 − 0.054 + 0.056 , and 958.7 − 5.9 + 6.3 days and masses of 9.14 − 0.63 + 0.65 , 11.0 ± 1, and 44.5 ± 2.9 Earth masses, respectively, with the planet d orbit significantly revised to over double that originally reported. We report two newly detected super-Earths, e and f, with periods of 4.31943 − 0.00068 + 0.00075 and 26.9 − 0.017 + 0.019 days and masses of 2.31 − 0.35 + 0.36 and 5.52 − 0.73 + 0.74 Earth masses, respectively. In addition, we identify a linear trend in the RV time series, and the cause of this acceleration is deemed to be a newly detected massive companion with a very long orbital period. HD 134606 now displays four low-mass planets in a compact region near the star, one gas giant further out in the habitable zone, an additional companion in the outer regime, and a low-mass M dwarf stellar companion at large separation, making it an intriguing target for system formation/evolution studies. The location of planet d in the habitable zone proves to be an exciting candidate for future space-based direct imaging missions, whereas continued RV observations of this system are recommended for understanding the nature of the massive, long-period companion.Peer reviewe
The NASA High-Resolution Speckle Interferometric Imaging Program: Validation and Characterization of Exoplanets and Their Stellar Hosts
Starting in 2008, NASA has provided the exoplanet community an observational program aimed at obtaining the highest resolution imaging available as part of its mission to validate and characterize exoplanets, as well as their stellar environments, in search of life in the Universe. Our current program uses speckle interferometry in the optical (320–1,000 nm) with new instruments on the 3.5-m WIYN and both 8-m Gemini telescopes. Starting with Kepler and K2 follow-up, we now support TESS and other space- and ground-based exoplanet related discovery and characterization projects. The importance of high-resolution imaging for exoplanet research comes via identification of nearby stellar companions that can dilute the transit signal and confound derived exoplanet and stellar parameters. Our observations therefore provide crucial information allowing accurate planet and stellar properties to be determined. Our community program obtains high-resolution imagery, reduces the data, and provides all final data products, without any exclusive use period, to the community via the Exoplanet Follow-Up Observation Program (ExoFOP) website maintained by the NASA Exoplanet Science Institute. This paper describes the need for high-resolution imaging and gives details of the speckle imaging program, highlighting some of the major scientific discoveries made along the way
TOI-733 b: A planet in the small-planet radius valley orbiting a Sun-like star
We report the discovery of a hot (Teq ≈ 1055 K) planet in the small-planet radius valley that transits the Sun-like star TOI-733. It was discovered as part of the KESPRINT follow-up program of TESS planets carried out with the HARPS spectrograph. TESS photometry from sectors 9 and 36 yields an orbital period of {equation presented} days and a radius of {equation presented}. Multi-dimensional Gaussian process modelling of the radial velocity measurements from HARPS and activity indicators gives a semi-amplitude of K = 2.23 ± 0.26 m s-1, translating into a planet mass of {equation presented}. These parameters imply that the planet is of moderate density ({equation presented}) and place it in the transition region between rocky and volatile-rich planets with H/He-dominated envelopes on the mass-radius diagram. Combining these with stellar parameters and abundances, we calculated planet interior and atmosphere models, which in turn suggest that TOI-733 b has a volatile-enriched, most likely secondary outer envelope, and may represent a highly irradiated ocean world. This is one of only a few such planets around G-type stars that are well characterised
A super-massive Neptune-sized planet
Neptune-sized planets exhibit a wide range of compositions and densities,
depending onf cators related to their formation and evolution history, such as
the distance from their host stars and atmospheric escape processes. They can
vary from relatively low-density planets with thick hydrogen-helium atmospheres
to higher-density planets with a substantial amount of water or a rocky
interior with a thinner atmosphere, such as HD 95338 b, TOI-849 b and TOI-2196
b. The discovery of exoplanets in the hot-Neptune desert, a region close to the
host stars with a deficit of Neptune-sized planets, provides insights into the
formation and evolution of planetary systems, including the existence of this
region itself. Here we show observations of the transiting planet TOI-1853 b,
which has a radius of 3.46 +- 0.08 Earth radii and orbits a dwarf star every
1.24 days. This planet has a mass of 73.2 +- 2.7 Earth masses, almost twice
that of any other Neptune-sized planet known so far, and a density of 9.7 +-
0.8 grams per cubic centimetre. These values place TOI-1853 b in the middle of
the Neptunian desert and imply that heavy elements dominate its mass. The
properties of TOI-1853 b present a puzzle for conventional theories of
planetary formation and evolution, and could be the result of several
proto-planet collisions or the final state of an initially high-eccentricity
planet that migrated closer to its parent star.Comment: Preprint submitted to Nature. Please refer to the published version
for the final parameters estimation
TESS Discovery of Twin Planets near 2:1 Resonance around Early M-Dwarf TOI 4342
With data from the Transiting Exoplanet Survey Satellite (TESS), we showcase
improvements to the MIT Quick-Look Pipeline (QLP) through the discovery and
validation of a multi-planet system around M-dwarf TOI 4342 (,
, , K,
pc). With updates to QLP, including a new multi-planet search, as well as
faster cadence data from TESS' First Extended Mission, we discovered two
sub-Neptunes ( and ; = 5.538 days and = 10.689 days)
and validated them with ground-based photometry, spectra, and speckle imaging.
Both planets notably have high transmission spectroscopy metrics (TSMs) of 36
and 32, making TOI 4342 one of the best systems for comparative atmospheric
studies. This system demonstrates how improvements to QLP, along with faster
cadence Full-Frame Images (FFIs), can lead to the discovery of new multi-planet
systems.Comment: accepted for publication in A
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