Relevant bibliographies by topics / Transiti planetari

Academic literature on the topic 'Transiti planetari'

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Published: 11 March 2023

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Journal articles on the topic "Transiti planetari"

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Heller, René, and Michael Hippke. "Signal preservation of exomoon transits during light curve folding." Astronomy & Astrophysics 657 (January 2022): A119. http://dx.doi.org/10.1051/0004-6361/202142403.

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In the search for moons around extrasolar planets (exomoons), astronomers are confronted with a stunning observation. Although 3400 of the 4500 exoplanets were discovered with the transit method and although there are well over 25 times as many moons than planets known in the Solar System (two of which are larger than Mercury), no exomoon has been discovered to date. In the search for exoplanet transits, stellar light curves are usually phase-folded over a range of trial epochs and periods. This approach, however, is not applicable in a straightforward manner to exomoons. Planet-moon transits either have to be modeled in great detail (including their orbital dynamics, mutual eclipses, etc.), which is computationally expensive, or key simplifications have to be assumed in the modeling. One such simplification is to search for moon transits outside of the planetary transits. The question we address in this report is how much in-transit data of an exomoon remains uncontaminated by the near-simultaneous transits of its host planet. We develop an analytical framework based on the probability density of the sky-projected apparent position of an exomoon relative to its planet and test our results with a numerical planet-moon transit simulator. For exomoons with planet-moon orbital separations similar to the Galilean moons, we find that only a small fraction of their in-transit data is uncontaminated by planetary transits: 14% for Io, 20% for Europa, 42% for Ganymede, and 73% for Callisto. The signal-to-noise ratio (S/N) of an out-of-planetary-transit folding technique is reduced compared to a full photodynamical model to about 38% (Io), 45% (Europa), 65% (Ganymede), and 85% (Callisto), respectively. For the Earth’s Moon, we find an uncontaminated data fraction of typically just 18% and a resulting S/N reduction to 42%. These values are astonishingly small and suggest that the gain in speed for any exomoon transit search algorithm that ignores the planetary in-transit data comes at the heavy price of losing a substantial fraction of what is supposedly a tiny signal in the first place. We conclude that photodynamical modeling of the entire light curve has substantial, and possibly essential, advantages over folding techniques of exomoon transits outside the planetary transits, in particular for small exomoons comparable to those of the Solar System.
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Wittrock, Justin M., Stefan Dreizler, Michael A. Reefe, Brett M. Morris, Peter P. Plavchan, Patrick J. Lowrance, Brice-Olivier Demory, et al. "Transit Timing Variations for AU Microscopii b and c." Astronomical Journal 164, no. 1 (June 30, 2022): 27. http://dx.doi.org/10.3847/1538-3881/ac68e5.

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Abstract We explore the transit timing variations (TTVs) of the young (22 Myr) nearby AU Mic planetary system. For AU Mic b, we introduce three Spitzer (4.5 μm) transits, five TESS transits, 11 LCO transits, one PEST transit, one Brierfield transit, and two transit timing measurements from Rossiter–McLaughlin observations; for AU Mic c, we introduce three TESS transits. We present two independent TTV analyses. First, we use EXOFASTv2 to jointly model the Spitzer and ground-based transits and obtain the midpoint transit times. We then construct an O − C diagram and model the TTVs with Exo-Striker. Second, we reproduce our results with an independent photodynamical analysis. We recover a TTV mass for AU Mic c of 10.8 − 2.2 + 2.3 M ⊕. We compare the TTV-derived constraints to a recent radial velocity (RV) mass determination. We also observe excess TTVs that do not appear to be consistent with the dynamical interactions of b and c alone or due to spots or flares. Thus, we present a hypothetical nontransiting “middle-d” candidate exoplanet that is consistent with the observed TTVs and candidate RV signal and would establish the AU Mic system as a compact resonant multiplanet chain in a 4:6:9 period commensurability. These results demonstrate that the AU Mic planetary system is dynamically interacting, producing detectable TTVs, and the implied orbital dynamics may inform the formation mechanisms for this young system. We recommend future RV and TTV observations of AU Mic b and c to further constrain the masses and confirm the existence of possible additional planet(s).
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Castellano, T., L. Doyle, and D. McIntosh. "The Visibility of Earth Transits." Symposium - International Astronomical Union 202 (2004): 445–47. http://dx.doi.org/10.1017/s0074180900218457.

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The recent photometric detection of planetary transits of the solar-like star HD 209458 at a distance of 47 parsecs suggest that transits can reveal the presence of Jupiter-size planetary companions in the solar neighborhood (Charbonneau et al. 2000; Henry et al. 2000). Recent space-based transit searches have achieved photometric precision within an order of magnitude of that required to detect the much smaller transit signal of an earth-size planet across a solar-size star. Laboratory experiments in the presence of realistic noise sources have shown that CCDs can achieve photometric precision adequate to detect the 9.6 E-5 dimming of the Sun due to a transit of the Earth (Borucki et al. 1997; Koch et al. 2000). Space-based solar irradiance monitoring has shown that the intrinsic variability of the Sun would not preclude such a detection (Borucki, Scargle, Hudson 1985). Transits of the Sun by the Earth would be detectable by observers that reside within a narrow band of sky positions near the ecliptic plane, if the observers possess current Earth epoch levels of technology and astronomical expertise. A catalog of solar-like stars that satisfy the geometric condition for Earth transit visibility are presented.
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Petrucci, Romina, Emiliano Jofré, Martín Schwartz, Andrea Buccino, and Pablo Mauas. "TTVs study in southern stars." Proceedings of the International Astronomical Union 7, S286 (October 2011): 441–44. http://dx.doi.org/10.1017/s1743921312005236.

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AbstractIn this contribution we present 4 complete planetary transits observed with the 40-cm telescope “Horacio Ghielmetti” located in San Juan(Argentina). These objects correspond to a continuous photometric monitoring program of Southern planet host-stars that we are carrying out since mid-2011. The goal of this project is to detect additional planetary mass objects around stars with known transiting-planets through Transit Timing Variations (TTVs). For all 4 transits the depth and duration are in good agreement with the values published in the discovery papers.
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Fernández-Lajús, Eduardo, Yamila Miguel, Andrea Fortier, and Romina P. Di Sisto. "Monitoring and analyzing exoplanetary transits from Argentina." Proceedings of the International Astronomical Union 6, S276 (October 2010): 416–17. http://dx.doi.org/10.1017/s174392131102059x.

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AbstractPhotometric observations of transits can be used to derive physical and orbital parameters of the system, like the planetary and stellar radius, orbital inclination and mean density of the star. Furthermore, monitoring possible periodic variations in transit timing of planets is important, since small changes can be caused by the presence of other planets or moons in the system. On the other hand, long term changes in the transit length can be due to the orbital precession of the planets. For these reasons we started an observational program dedicated to observe transits of known exoplanets with the aim of contributing to a better understanding of these planetary systems. In this work we present our first results obtained using the observational facilities in Argentina including the 2.15 telescope at CASLEO.
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Hazra, Soumitra, Ofer Cohen, and Igor V. Sokolov. "Exoplanet Radio Transits as a Probe for Exoplanetary Magnetic Fields—Time-dependent MHD Simulations." Astrophysical Journal 936, no. 2 (September 1, 2022): 144. http://dx.doi.org/10.3847/1538-4357/ac8978.

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Abstract We perform a series of time-dependent magnetohydrodynamic simulations of the HD 189733 star–planet system in order to predict radio transit modulations due to the interaction between the stellar wind and planetary magnetic field. The simulation combines a model for the stellar corona and wind with an exoplanet that is orbiting the star in a fully dynamic, time-dependent manner. Our simulations generate synthetic radio images that enable us to obtain synthetic radio light curves in different frequencies. We find a clear evidence for the planetary motion in the radio light curves. Moreover, we find specific repeated features in the light curves that are attributed to the passage of the planetary magnetosphere in front of the star during transit. More importantly, we find a clear dependence in magnitude and phase of these light-curve features on the strength of the planetary magnetic field. Our work demonstrates that if radio transits could be observed, they could indeed provide information about the magnetic field strength of the transiting exoplanet. Future work to parameterize these light-curve features and their dependence on the planetary field strength would provide tools to search for these features in radio observation data sets. As we only consider the thermal radio emission from the host star for our study, very sensitive radio interferometers are necessary to detect these kinds of planetary transits in radio.
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Kostogryz, N. M., T. M. Yakobchuk, and A. P. Vidmachenko. "Polarimetry of Exoplanetary System CoRoT-2." Proceedings of the International Astronomical Union 7, S282 (July 2011): 209–10. http://dx.doi.org/10.1017/s1743921311027396.

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AbstractWe present the results of modelling the polarization resulting from the planetary transits and stellar spots in the system Corot-2 using the Monte Carlo method. The planetary transit was estimated to produce a polarization maximum at the limb of ~5 × 10−6, adopting solar center-to-limb polarization. Assuming different parameters of the spots, we evaluated the flux and polarization changes due to the stellar activity.
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Emilio, Marcelo, Rock Bush, Jeff Kuhn, and Isabelle Scholl. "Solar astrometry with planetary transits." Proceedings of the International Astronomical Union 15, S354 (June 2019): 481–93. http://dx.doi.org/10.1017/s1743921320004068.

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AbstractPlanetary transits are used to measure the solar radius since the beginning of the 18th century and are the most accurate direct method to measure potentially long-term variation in the solar size. Historical measures present a range of values dominated by systematic errors from different instruments and observers. Atmospheric seeing and black drop effect contribute as error sources for the precise timing of the planetary transit ground observations. Both Solar and Heliospheric Observatory (SOHO) and Solar Dynamics Observatory (SDO) made observations of planetary transits from space to derive the solar radius. The International Astronomical Union approved the resolution B3 in 2015, defining a nominal solar radius of precisely 695,700 km. In this work, we show that this value is off by more than 300 km, which is one order of magnitude higher than the error of the most recent solar radius observations.
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Winn, Joshua N. "Measuring accurate transit parameters." Proceedings of the International Astronomical Union 4, S253 (May 2008): 99–109. http://dx.doi.org/10.1017/s174392130802629x.

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AbstractBy observing the transits of exoplanets, one may determine many fundamental system parameters. I review current techniques and results for the parameters that can be measured with the greatest precision, specifically, the transit times, the planetary mass and radius, and the projected spin-orbit angle.
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Vissapragada, Shreyas, Gudmundur Stefánsson, Michael Greklek-McKeon, Antonija Oklopčić, Heather A. Knutson, Joe P. Ninan, Suvrath Mahadevan, et al. "A Search for Planetary Metastable Helium Absorption in the V1298 Tau System." Astronomical Journal 162, no. 5 (November 1, 2021): 222. http://dx.doi.org/10.3847/1538-3881/ac1bb0.

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Abstract Early in their lives, planets endure extreme amounts of ionizing radiation from their host stars. For planets with primordial hydrogen and helium-rich envelopes, this can lead to substantial mass loss. Direct observations of atmospheric escape in young planetary systems can help elucidate this critical stage of planetary evolution. In this work, we search for metastable helium absorption—a tracer of tenuous gas in escaping atmospheres—during transits of three planets orbiting the young solar analog V1298 Tau. We characterize the stellar helium line using HET/HPF, and find that it evolves substantially on timescales of days to months. The line is stable on hour-long timescales except for one set of spectra taken during the decay phase of a stellar flare, where absoprtion increased with time. Utilizing a beam-shaping diffuser and a narrowband filter centered on the helium feature, we observe four transits with Palomar/WIRC: two partial transits of planet d (P = 12.4 days), one partial transit of planet b (P = 24.1 days), and one full transit of planet c (P = 8.2 days). We do not detect the transit of planet c, and we find no evidence of excess absorption for planet b, with ΔR b/R ⋆ < 0.019 in our bandpass. We find a tentative absorption signal for planet d with ΔR d/R ⋆ = 0.0205 ± 0.054, but the best-fit model requires a substantial (−100 ± 14 minutes) transit-timing offset on a two-month timescale. Nevertheless, our data suggest that V1298 Tau d may have a high present-day mass-loss rate, making it a priority target for follow-up observations.
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Dissertations / Theses on the topic "Transiti planetari"

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Giacobbe, Paolo. "Photometric transit search for planets around cool stars from the Western Italian Alps: the APACHE survey." Doctoral thesis, Università degli studi di Trieste, 2014. http://hdl.handle.net/10077/9965.

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2012/2013
Small-size ground-based telescopes can effectively be used to look for transiting rocky planets around nearby low-mass M stars using the photometric transit method. Since 2008, a consortium of the Astrophysical Observatory of Torino (OATo-INAF) and the Astronomical Observatory of the Autonomous Region of Aosta Valley (OAVdA) have been preparing for the long-term photometric survey APACHE (A PAthway toward the Characterization of Habitable Earths), aimed at finding transiting small-size planets around thousands of nearby early and mid-M dwarfs. APACHE uses an array of five dedicated and identical 40-cm Ritchey-Chretien telescopes and its routine science operations started at the beginning of summer 2012. Here I present the results of the `pilot study', a year-long photometric monitoring campaign of a sample of 23 nearby dM stars, and of the APACHE survey first year data. In these studies, I set out to (i) demonstrate the sensitivity to > 2 Rearth transiting planets with periods of up to a few days around our programme stars, through a two-fold approach that combines a characterization of the statistical noise properties of our photometry with the determination of transit detection probabilities via simulations; and (ii), where possible, improves our knowledge of some astrophysical properties (e.g. activity, rotation) of our targets by combining our differential photometric measurements with spectroscopic information from the long-term programme GAPS with the HARPS-N spectrograph on the Telescopio Nazionale Galileo. Furthermore, cool M dwarfs within a few tens of parsecs from the Sun are becoming the focus of dedicated observational programs in the realm of exoplanet astrophysics that will make use of astrometric measurements. I present numerical simulations to gauge the Gaia potential for precision astrometry of exoplanets orbiting a sample of known dM stars within ~ 30 pc from the Sun. I then investigate some aspects of the synergy between the astrometric data expected from the Gaia mission on nearby M dwarfs and the APACHE program.
XXV Ciclo
1985
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Aigrain, Suzanne. "Planetary transits and stellar variability." Thesis, University of Cambridge, 2005. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.614684.

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McQuillan, Amy. "Stellar variability and rotation in Kepler planetary transit search data." Thesis, University of Oxford, 2013. http://ora.ox.ac.uk/objects/uuid:802a873d-650f-4f0b-b814-f8397b2798e2.

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The recent space-based exoplanet transit searches, CoRoT and Kepler, have revolutionised the field of stellar variability. In this thesis I exploit the public Kepler data to characterise stellar variability, and study rotation periods. For the study of stellar variability it is a complicated but necessary process to remove instrumental systematics while maintaining intrinsic stellar signal. I was involved in the development of a new correction method for systematics, denoted ARC (Astrophysically Robust Correction). This method relies on the removal of a set of basis functions that are determined to be present in small amounts across many light curves. Using the first month of Kepler data, corrected with the ARC method, I studied the variability properties of main sequence stars as a function of fundamental stellar parameters. I find that the fraction of stars with variability greater than that of the Sun is 60%, and confirm the trend of increasing variability with decreasing effective temperatures. I show tentative evidence that the more active stars have lower proper motions and may be located closer to the galactic plane. I also investigate the frequency content of the variability, showing that there exist significant differences in the nature of variability between spectral types, with a trend towards longer periods at later spectral types. In order to exploit the full potential of the Kepler data for stellar rotation period measurement, I developed a novel method of period detection for use on star spot modulated light curves. Standard approaches to period detection are based on Fourier decomposition or least-squares fitting of sinusoidal models. However, typical stellar light curves are neither sinusoidal nor strictly periodic. Therefore, I developed an algorithm for period detection based on the autocorrelation function (ACF) of the light curve. Because the ACF measures only the degree of self-similarity of the light curve at a given time lag, the period remains detectable even when the amplitude and phase of the photometric modulation evolve significantly. I applied the ACF method for the sample of M-dwarfs observed during the first 10 months of the Kepler mission, and detected rotation periods in 1570, ranging from 0.37-69.7 days. The rotation period distribution is clearly bimodal, with peaks at ~19 and ~33 days, hinting at two distinct waves of star formation. These two peaks form two distinct sequences in period-temperature space, with the period decreasing with increasing temperature. In a natural continuation to this work I applied measured periods for 1000 stars in each of the F, G and K-dwarf sets observed by Kepler, and combined these with the M-dwarf results. The trend of increasing rotation period with increasing mass is clear throughout, as the observations fall along a wide by distinct sequence. Comparison to the rotational isochrones of Barnes (2007) show an overall agreement, although the dataset, which I believe is the largest set of rotation period measurements for main sequence stars, shows addition detail, not captured by the gyrochronology relations. This includes a dip in the rotation period distribution at ~0.6 M⊙ and a steep increase in period for the M-dwarfs. I also applied the ACF method to the Kepler exoplanet candidate host stars and used the results to search for evidence of tidal interaction between the star and planet. I show that for the majority of exoplanet host stars, spin-orbit interaction will not have affected the stellar rotation period, permitting the application of gyrochronology for age determination. A comparison of the host stars with a sample of field stars selected to match their temperature and magnitude distribution also indicates no significant difference in the period or amplitude distributions of the two sets. The only notable variation is the lack of planets around the very fast rotators across all spectral types.
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De, Marchi Fabrizio. "Variable stars and planetary transit search in super metal-rich open clusters." Doctoral thesis, Università degli studi di Padova, 2008. http://hdl.handle.net/11577/3427100.

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This PhD thesis presents the analysis of a large sample of photometric data relative to the super metal-rich open clusters NGC6791 and NGC6253. The main goal of the surveys was the search for extrasolar planets using the transits method. I contributed to the extrasolar planet search by making numerical simulations in order to estimate the number of expected transiting planets. Moreover I analyzed the entire sample of light curves in order to find variable stars. I discovered 260 new variable stars in the field of NGC6791 and 597 in the field of NGC6253. The classification of all variables is presented and discussed in this work.
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Street, Rachel. "A search for extra-solar planetary transits in the field of open cluster NGC 6819." Thesis, University of St Andrews, 2002. http://hdl.handle.net/10023/12939.

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The technique of searching for extra-solar planetary transits is investigated. This technique, which relies on detecting the brief, shallow eclipses caused by planets passing across the line of sight to the primary star, requires high-precision time-series photometry of large numbers of stars in order to detect these statistically rare events. Observations of ~ 18000 stars in the field including the intermediate-age open cluster NGC 6819 are presented. This target field contrasts with the stellar environment surveyed by the radial velocity technique, which concentrates on the Solar neighbourhood. I present the data-reduction techniques used to obtain high-precision photometry in a semi-automated fashion for tens of thousands of stars at a time, together with an algorithm designed to search the resulting lightcurves for the transit signatures of hot Jupiter type planets. I describe simulations designed to test the detection efficiency of this algorithm and, for comparison, predict the number of transits expected from this data, assuming that hot Jupiter planets similar to HD 209458 are as common in the field of NGC 6819 as they are in the Solar neighbourhood. While no planetary transits have yet been identified, the detection of several very low amplitude eclipses by stellar companions demonstrates the effectiveness of the method. This study also indicates that stellar activity and particularly blending are significant causes of false detections. A useful additional consequence of studying this time-series photometry is the census it provides of some of the variable stars in the field. I report on the discovery of a variety of newly-discovered variables, including Algol-type detached eclipsing binaries which are likely to consist of M-dwarf stars. Further study of these stars is strongly recommended in order to help constrain models of stellar structure at the very low mass end. I conclude with a summary of this work in the context of other efforts being made in this field and recommend promising avenues of further study.
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Ballerini, Paola. "Effects of starspots activity on optical and near infrared observations of planetary transits." Doctoral thesis, Università di Catania, 2013. http://hdl.handle.net/10761/1377.

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In this thesis, I report on the effects that magnetic stellar activity of solar-type stars induces on stellar light curves involved in the photometric technique for the detection and characterization of transiting extra-solar planets that is one of the most effective detection methods, the first being the radial velocity technique. Stellar magnetic activity is a source of noise in the study of the transits of extra-solar planets since it induces flux variations that significantly affect the transit depth determination and the derivations of planetary and stellar parameters. Surface brightness inhomogeneities, such as starspots or bright faculae, on star disc have an intrinsic dependence on wavelength and thus on the stellar colours. The colour dependence of stellar activity may significantly influence the characterization of planetary atmospheres since it produces stellar flux variations that may mimic those due to the presence of molecular or atomic species in the transmitted planetary spectra. In this thesis I focus on the effects due essentially to stellar spots present in the visible hemisphere of solar-type stars. The proposed method is a theoretical one, aiming to predict the starspot-induced effects with the use of stellar atmospheric models and I present a systematic approach to quantify the corresponding stellar flux variations as a function of wavelength bands. Therefore I consider a star with spots covering a given fraction of its disc and model the variability in both the UBVRIJHK photometric system and the Spitzer/IRAC wavebands for dwarf stars from G to M spectral types. Then I compare starspot-induced flux variations in these different passbands with planetary transits and quantify how they affect the determination of the planetary radius and the analysis of the transmission spectroscopy in the study of planetary atmospheres. My results suggest that the monitoring of the systems by using broad-band photometry, from visible to infrared, helps to constrain spots effects by estimating the R parameter, i.e. the ratio of the relative variations in the stellar fluxes at short wavelength optical bands (e.g., U or B) to near-infrared ones (e.g., J or K). Its numerical value can be used to distinguish starspot brightness dips from planetary transits in a single stellar light curve. In addition to the perturbations in the measurement of the planetary radius, the perturbations in the transit light curve profiles due to starspots can affect the determinations of orbital parameters, i.e., the relative semi-major axis and the inclination of the planetary orbit, that are directly derived by fitting procedure of the transit light curves. These distortions in the transit light curves have a significant impact on the derivation of stellar parameters and, above all, on the stellar density thus bothering the stellar evolutionary estimates. The results derived from the synthetic photometric analysis are presented and discussed in Ballerini et al. 2012.
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Nisley, Ishara. "Transit timing variations of the exoplanet K2-25b." Thesis, Massachusetts Institute of Technology, 2017. http://hdl.handle.net/1721.1/117447.

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Thesis: S.B., Massachusetts Institute of Technology, Department of Earth, Atmospheric, and Planetary Sciences, 2017.
Cataloged from PDF version of thesis. "May 16, 2017." "This thesis was submitted to the Institute Archives without all the required signatures"--Disclaimer Notice page.
Includes bibliographical references (page 53).
Transit light curves of the exoplanet K2-25b were studied to examine the possibility of transit timing variations (TTVs) in the system, which could imply the presence of a perturbing planet. Observations of K2-25b transits were taken using 14-inch and 24-inch telescopes at Wallace Astrophysical Observatory. Two transit light curves were fit using an MCMC implementation to find the orbital period, planetary radius, and semi-major axis. A new period calculation yielded an orbital period of 3.48457 +/-0.00004, consistent with the period of 3.484552 +0.000044/-0.000036 from Mann et al. 2016. No significant variations were found in the midtimes of the new transit observations when comparing them to the midtime originally published in Mann et al. 2016. Future observations will require smaller uncertainties to meaningfully constrain the mass and period of potential perturbing planets. Signal-to-noise ratio calculations showed that telescopes over approximately 2.2 meters in diameter have better potential to detect small TTVs.
by Ishara Nisley.
S.B.
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Adams, Elisabeth Rose. "Transit timing with fast cameras on large telescopes." Thesis, Massachusetts Institute of Technology, 2010. http://hdl.handle.net/1721.1/59737.

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Thesis (Ph. D.)--Massachusetts Institute of Technology, Dept. of Earth, Atmospheric, and Planetary Sciences, 2010.
Cataloged from PDF version of thesis.
Includes bibliographical references (p. 171-178).
Timing and system parameters were measured for seven transiting exoplanets: OGLETR- 56b (11 transits), OGLE-TR-132b (7), OGLE-TR-111b (6), OGLE-TR-113b (6), CoRoT-2b (3), OGLE-TR-10b (3), and XO-2b (2). Ground-based observations of 38 transits were made using three new frame-transfer instruments: POETS and MagICe2v on the 6.5m Magellan telescopes, and MORIS on the 3m IRTF. For each planet, all transit light curves including available literature data were jointly fit using a Monte Carlo Markov Chain method, providing accurate new values for the planetary radius and other parameters. Transit ephemerides have been updated and transit midtimes have been investigated for potential transit timing variations (TTVs) caused by other planets or moons. Our transit midtime analysis contradicts a claimed TTV for OGLE-TR-111b (Diaz et al., 2008), finding no evidence in data from 2005-2009. The radius, 1.019 + 0.026 Rj, is intermediate to previous values (Winn et al., 2007; Diaz et al., 2008). We confirm the radius of OGLE-TR-56b, which previously had only one light curve (Pont et al., 2007), as 1.332 ± 0.063 Rj, but find a longer duration by 15 minutes, while the orbital period, 1.2119094 ± 0.0000024, is unchanged. Times for OGLE-TR-10b are consistent with the ephemeris of Holman et al. (2007), though two literature transits show large deviations (586 ± 86 s; Pont et al., 2007) and (-612 ± 26 s; Bentley et al., 2009). Times for four planets (OGLE-TR-113b, OGLE-TR-132b, CoRoT-2b, and XO-2b), with midtime errors as small as 9 s, agree with published ephemerides and show no signs of TTVs. The orbital period of OGLE-TR-113b derived from new data from 2007-2009, however, is shorter by 0.24 ± 0.12 s compared to the period calculated for literature data from 2002 and 2005. If confirmed, this would be the first detection of a change in the orbital period of an exoplanet, which could be caused by orbital decay as the planet falls onto its star.
by Elisabeth Rose Adams.
Ph.D.
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Morley, Caroline V. "Measuring transit timing variations of exoplanets using small telescopes." Thesis, Massachusetts Institute of Technology, 2010. http://hdl.handle.net/1721.1/114139.

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Thesis: S.B., Massachusetts Institute of Technology, Department of Earth, Atmospheric, and Planetary Sciences, 2010.
Cataloged from PDF version of thesis.
Includes bibliographical references (pages 57-58).
Transits of exoplanets were observed from June 2009 through January 2010. Six transit light curves are presented in this paper for three planets: WASP-10b, WASP- 11/HAT-P-10b, and TrES-3. Measurements of the planetary radii, semi-major axis, transit duration, and period confirmed literature values to within two sigma. Transit timing variations were not observed in these systems, but calculations show that it would be possible to measure transit timing variations induced by large exomoons (greater than about 6 Earth masses) in the WASP-11/HAT-P-10b system. Challenges of exoplanet observation from small telescopes are discussed. It was determined that overall, transit measurements of many exoplanets using small telescopes can be successful and scientifically useful.
by Caroline V. Morley.
S.B.
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DeCroix, David Scot. "Large-eddy Simulations of the Convective and Evening Transition Planetary Boundary Layers." NCSU, 2001. http://www.lib.ncsu.edu/theses/available/etd-20010319-182404.

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Large-eddy simulation (LES) is a very useful tool in computationalfluid dynamics. The LES model allows one to solve a filtered set of theNavier-Stokes equations, thereby explicitly resolving scales of motionlarger than the discretization or grid size. Those motions smaller thanthe grid size are parameterized using a so-called subgrid scale model.

In this series of papers, we will use the TASS LES model, originallya cloud model, which has been modified to simulate planetary boundarylayer turbulence. We will first introduce the LES model and a newgrid-nesting method for the LES. Then we will present simulations ofthe convective planetary boundary layer, and then use the LES to studythe decay of convective planetary boundary layer turbulence to a stablystratified state.

The LES model has been modified to include a grid nesting capability.Grid meshes of higher resolution may be embedded within the LES enablingone to resolve smaller scales of motion (turbulence) than would bepossible by using a single grid mesh. The grid nesting methodology isdescribed in detail in Chapter 2.

In Chapter 3, the nested-grid LES will be applied to thesimulation of the convective planetary boundary layer. We will usea total of three grid meshes to increase the resolution in the surfacelayer, allowing a detailed analysis of the turbulence near the surface ofthe earth.

In Chapter 4, we will focus on applying Rayleigh Benardconvection criteria, using a linearized perturbation method,to the surface layer of a CBL produced by large-eddy simulation.Similarities and differences will be discussed between the LESproduced surface layer and classical Rayleigh-Benard convection theory.

In Chapter 5, using a large-eddy simulation model, we willexamine in detail the turbulent kinetic energy (TKE) budget during theevening transition. The simulation will be performed in order to compareto observations gathered at the Dallas-Fort Worth International Airport,Fort-Worth, TX. during September and October 1997.

In Chapter 6 the decay of planetary boundary layerturbulence during the evening transition will be studied. In previousstudies of the decay of turbulence, the effects of mean winds and shearsdue to pressure gradient on the turbulence decay was not considered.We propose to examine the effects of increasing geostrophic wind onthe convective boundary layer and its transition or decay to a stablecondition. Finally, the overall conclusions of each chapter will bepresented.

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Books on the topic "Transiti planetari"

1

Sandford, Emily Ruth. The Shapes of Planet Transits and Planetary Systems. [New York, N.Y.?]: [publisher not identified], 2020.

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L, Grove Timothy, and United States. National Aeronautics and Space Administration., eds. Partitioning of moderately siderophile elements among olivine, silicate melt, and sulfide melt: Constraints on core formation in the earth and Mars. [Washington, DC: National Aeronautics and Space Administration, 1997.

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Kent, April Elliott. Astrological transits: The beginner's guide to using planetary cycles to plan and predict your day, week, year (or destiny). Beverly, MA: Fair Winds Press, 2015.

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Valdivia-Silva, Julio. Planetary conditions at the Hadean and Archean transition: Possible scenarios for the origin of life. New York: Nova Science Publisher's, Inc., 2011.

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United States. National Aeronautics and Space Administration., ed. The transition from diapirism to dike intrustion: Implications for planetary volcanism, status report, 04-01-93 - 03-31-94. [Washington, DC: National Aeronautics and Space Administration, 1994.

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Yuh-Lang, Lin, and United States. National Aeronautics and Space Administration., eds. Numerical modeling studies of wake vortex transport and evolution within the planetary boundary layer: NASA grant NCC-1-188 : FY 97 annual report. [Washington, DC: National Aeronautics and Space Administration, 1998.

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Franco, Divaldo Pereira, Miranda, Manoel Philomeno de. Planetary Transition. Leal Publisher INC, 2016.

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Sepharial. Transits and Planetary Periods. Kessinger Publishing, LLC, 2007.

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Sepharial. The Tables Of Houses And Planetary Transits - Pamphlet. Kessinger Publishing, LLC, 2006.

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(Editor), Editorial Kier, and Graciela Goldsmidt (Illustrator), eds. El Misterio De La Cruz En La Actual Transicion Planetaria/ The Mystery of the Cross in the Present Planetary Transition (Trigueirinho). 2nd ed. Kier Editorial, 2004.

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Book chapters on the topic "Transiti planetari"

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Cameron, Andrew Collier. "Extrasolar Planetary Transits." In Methods of Detecting Exoplanets, 89–131. Cham: Springer International Publishing, 2016. http://dx.doi.org/10.1007/978-3-319-27458-4_2.

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Leone, Giovanni. "Transition Topography (Mars)." In Encyclopedia of Planetary Landforms, 1–6. New York, NY: Springer New York, 2014. http://dx.doi.org/10.1007/978-1-4614-9213-9_650-1.

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Leone, Giovanni. "Transition Topography (Mars)." In Encyclopedia of Planetary Landforms, 2169–73. New York, NY: Springer New York, 2015. http://dx.doi.org/10.1007/978-1-4614-3134-3_650.

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Van de Steene, G. C., and P. A. M. van Hoot. "Infrared Observations of Candidate Post-AGB Transition Objects." In Planetary Nebulae, 372. Dordrecht: Springer Netherlands, 1997. http://dx.doi.org/10.1007/978-94-011-5244-0_182.

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Gaigalas, G., R. Kisielius, G. Merkelis, and M. Vilkas. "E2 and M1 Transition Probabilities in Ions of the Nitrogen Isoelectronic Sequence Calculated Using MBPT." In Planetary Nebulae, 95. Dordrecht: Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-2088-3_35.

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Barros, Susana, and João P. Faria. "Tutorial: Detecting Planetary Transits and Radial-Velocity Signals." In Astrophysics and Space Science Proceedings, 267–74. Cham: Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-59315-9_15.

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Kwok, Sun. "Transition from Red Giants to Planetary Nebulae." In Late Stages of Stellar Evolution, 321–35. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3813-7_52.

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Clammer, John. "The Cultural and Civilizational Roots of Our Planetary Crisis." In Cultures of Transition and Sustainability, 1–22. New York: Palgrave Macmillan US, 2016. http://dx.doi.org/10.1057/978-1-137-52033-3_1.

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Vanderburg, Andrew, and Saul A. Rappaport. "Transiting Disintegrating Planetary Debris Around WD 1145+017." In Handbook of Exoplanets, 1–24. Cham: Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-30648-3_37-1.

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Vanderburg, Andrew, and Saul A. Rappaport. "Transiting Disintegrating Planetary Debris Around WD 1145+017." In Handbook of Exoplanets, 2603–26. Cham: Springer International Publishing, 2018. http://dx.doi.org/10.1007/978-3-319-55333-7_37.

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Conference papers on the topic "Transiti planetari"

1

Engeling, K. W., M. Shah, R. P. Pitts, M. M. Tessema, G. D. Massa, A. Meier, D. Rinderknecht, et al. "Plasma for Crewed Transit and Planetary Habitation." In 2021 IEEE International Conference on Plasma Science (ICOPS). IEEE, 2021. http://dx.doi.org/10.1109/icops36761.2021.9588578.

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Kopp, Greg. "Liquid crystal intensity modulator for simulating planetary transits." In Optical Science and Technology, SPIE's 48th Annual Meeting, edited by Daniel R. Coulter. SPIE, 2003. http://dx.doi.org/10.1117/12.504521.

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Schultz, A. B. "HST/FGS Photometry of Planetary Transits of HD 209458." In THE SEARCH FOR OTHER WORLDS: Fourteenth Astrophysics Conference. AIP, 2004. http://dx.doi.org/10.1063/1.1774516.

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Schneider, Steven. "Laminar-Turbulent Transition on Reentry Capsules and Planetary Probes." In 35th AIAA Fluid Dynamics Conference and Exhibit. Reston, Virigina: American Institute of Aeronautics and Astronautics, 2005. http://dx.doi.org/10.2514/6.2005-4763.

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SIGISMONDI, C., X. WANG, P. ROCHER, and E. REIS NETO. "VENUS TRANSITS: HISTORY AND OPPORTUNITIES FOR PLANETARY, SOLAR AND GRAVITATIONAL PHYSICS." In Proceedings of the MG13 Meeting on General Relativity. WORLD SCIENTIFIC, 2015. http://dx.doi.org/10.1142/9789814623995_0443.

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CANAVAN, GREGORY H. "TRANSITION FROM ADVERSARIAL TO COOPERATIVE INTERACTION." In Proceedings of the International Seminar on Nuclear War and Planetary Emergencies — 26th Session. WORLD SCIENTIFIC, 2002. http://dx.doi.org/10.1142/9789812776945_0009.

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Abdulmyanov, T. "Comparison of the dynamics of Jupiter’s coorbital asteroids and the dynamics of bodies in debris disks." In ASTRONOMY AT THE EPOCH OF MULTIMESSENGER STUDIES. Proceedings of the VAK-2021 conference, Aug 23–28, 2021. Crossref, 2022. http://dx.doi.org/10.51194/vak2021.2022.1.1.018.

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The mechanisms of fragmentation of the equatorial dust disk around young stars and the formation of planetary systemsare considered. Using the model of librational motions of co-orbital asteroids of Jupiter, a model of viscous motion of gas,dust particles and small bodies in dust disks is constructed. The dynamic viscosity is obtained from the Navier-Stokesequation for three cases of characteristic flow orbits.It is shown that the librational orbits of Trojans at the early stages ofthe evolution of planetary systems could be transit orbits for dust particles during the formation of celestial bodies of smalland large sizes and masses.
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ZHANG, XILIANG. "TECHNOLOGIES AND POLICIES FOR THE TRANSITION TO LOW CARBON ENERGY SYSTEM IN CHINA." In International Seminar on Nuclear War and Planetary Emergencies 42nd Session. WORLD SCIENTIFIC, 2010. http://dx.doi.org/10.1142/9789814327503_0033.

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EICHHAMMER, WOLFGANG. "MAKING RAPID TRANSITION TO AN ENERGY SYSTEM CENTERED ON ENERGY EFFICIENCY AND RENEWABLES POSSIBLE." In International Seminar on Nuclear War and Planetary Emergencies 42nd Session. WORLD SCIENTIFIC, 2010. http://dx.doi.org/10.1142/9789814327503_0022.

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Guo, Yi, and Robert G. Parker. "Effects of Bearing Radial Internal Clearance on Dynamic Behavior and Bifurcations in Planetary Gears." In ASME 2011 International Design Engineering Technical Conferences and Computers and Information in Engineering Conference. ASMEDC, 2011. http://dx.doi.org/10.1115/detc2011-48891.

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This study investigates the dynamics of planetary gears where nonlinearity is induced by bearing clearance. Lumped-parameter and finite element models of planetary gears with bearing clearance, tooth separation, and gear mesh stiffness variation are developed. The harmonic balance method with arc-length continuation is used to obtain the dynamic response of the lumped-parameter model. Solution stability is analyzed using Floquet theory. Rich nonlinear behavior is exhibited in the dynamic response, consisting of nonlinear jumps and a hardening effect induced by the transition from no bearing contact to contact. The bearings of the central members (sun, ring, and carrier) impact against the bearing races near resonance, which leads to coexisting solutions in wide speed ranges, grazing bifurcation, and chaos. Secondary Hopf bifurcation is the route to chaos. Input torque can significantly suppress the nonlinear effects caused by bearing clearance.
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