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Journal articles on the topic 'Transit depth'

Author: Grafiati

Published: 3 June 2025

Last updated: 19 July 2025

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1

Cherdwongsung, P., S. Awiphan, P. Kittara, K. Matan, and N. Nakharutai. "Detectability of exomoons by examining the signals from a model of transiting exoplanets with moons." Journal of Physics: Conference Series 2145, no. 1 (2021): 012009. http://dx.doi.org/10.1088/1742-6596/2145/1/012009.

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Abstract Exomoons are natural satellites of exoplanets. Nowadays, none has been confirmed. However, a number of detection techniques have been proposed, including Transit Timing Variations (TTV) and Transit Duration Variations (TDV) techniques. From a recent study, fitting observed transit with the traditional photocentric fitting model shows unique features around the primary and secondary exomoon transits in TDV and transit depth signals, which might reduce the detectability. The aim of this work is to retrieve the variation of TTV, TDV and transit depth signals of exomoon systems with the p

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Mallonn, M., K. Poppenhaeger, T. Granzer, M. Weber, and K. G. Strassmeier. "Detection capability of ground-based meter-sized telescopes for shallow exoplanet transits." Astronomy & Astrophysics 657 (January 2022): A102. http://dx.doi.org/10.1051/0004-6361/202140599.

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Meter-sized ground-based telescopes are frequently used today for the follow-up of extrasolar planet candidates. While the transit signal of a Jupiter-sized object can typically be detected to a high level of confidence with small telescope apertures as well, the shallow transit dips of planets with the size of Neptune and smaller are more challenging to reveal. We employ new observational data to illustrate the photometric follow-up capabilities of meter-sized telescopes for shallow exoplanet transits. We describe in detail the capability of distinguishing the photometric signal of an exoplan

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Alapini, Aude, and Suzanne Aigrain. "Reconstruction of the transit signal in the presence of stellar variability." Proceedings of the International Astronomical Union 3, S249 (2007): 89–92. http://dx.doi.org/10.1017/s174392130801644x.

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AbstractIntrinsic stellar variability can hinder the detection of shallow transits, particularly in space-based data. Therefore, this variability has to be filtered out before running the transit search. Unfortunately, filtering out the low frequency signal of the stellar variability also modifies the transit shape. This results in errors in the measured transit depth and duration used to derive the planet radius, and orbital inclination. We present an evaluation of the magnitude of this effect based on 20 simulated light curves from the CoRoT blind exercise 2 (BT2). We then present an iterati

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Heller, René. "Analytic solutions to the maximum and average exoplanet transit depth for common stellar limb darkening laws." Astronomy & Astrophysics 623 (March 2019): A137. http://dx.doi.org/10.1051/0004-6361/201834620.

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Context. The depth of an exoplanetary transit in the light curve of a distant star is commonly approximated as the squared planet-to-star radius ratio, (Rp/Rs)2. Stellar limb darkening, however, can result in significantly deeper transits. An analytic solution would be worthwhile to illustrate the principles of the problem and predict the actual transit signal required for the planning of transit observations with certain signal-to-noise requirements without the need of computer-based transit simulations. Aims. We calculate the overshoot of the mid-transit depth caused by stellar limb darkenin

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Oddo, Dominic, Diana Dragomir, Alexis Brandeker, et al. "Characterization of a Set of Small Planets with TESS and CHEOPS and an Analysis of Photometric Performance." Astronomical Journal 165, no. 3 (2023): 134. http://dx.doi.org/10.3847/1538-3881/acb4e3.

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Abstract The radius valley carries implications for how the atmospheres of small planets form and evolve, but this feature is visible only with highly precise characterizations of many small planets. We present the characterization of nine planets and one planet candidate with both NASA TESS and ESA CHEOPS observations, which adds to the overall population of planets bordering the radius valley. While five of our planets—TOI 118 b, TOI 262 b, TOI 455 b, TOI 560 b, and TOI 562 b—have already been published, we vet and validate transit signals as planetary using follow-up observations for four n

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Zuckerman, Anna, James R. A. Davenport, Steve Croft, Andrew Siemion, and Imke de Pater. "The Breakthrough Listen Search for Intelligent Life: Detection and Characterization of Anomalous Transits in Kepler Lightcurves." Astronomical Journal 167, no. 1 (2023): 20. http://dx.doi.org/10.3847/1538-3881/acfa6c.

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Abstract Never before has the detection and characterization of exoplanets via transit photometry been as promising and feasible as it is now, due to the increasing breadth and sensitivity of time domain optical surveys. Past works have made use of phase-folded stellar lightcurves in order to study the properties of exoplanet transits because this provides the highest signal that a transit is present at a given period and ephemeris. Characterizing transits on an individual, rather than phase-folded, basis is much more challenging due to the often low signal-to-noise ratio of lightcurves, missi

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Gondhalekar, Yash, Eric D. Feigelson, Gabriel A. Caceres, Marco Montalto, and Snehanshu Saha. "A Study of Two Periodogram Algorithms for Improving the Detection of Small Transiting Planets." Astrophysical Journal Letters 959, no. 2 (2023): L16. http://dx.doi.org/10.3847/2041-8213/ad0844.

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Abstract The sensitivities of two periodograms are compared for weak signal planet detection in transit surveys: the widely used Box Least Squares (BLS) algorithm following light curve detrending and the Transit Comb Filter (TCF) algorithm following autoregressive ARIMA modeling. Small depth transits are injected into light curves with different simulated noise characteristics. Two measures of spectral peak significance are examined: the periodogram signal-to-noise ratio (S/N) and a false alarm probability (FAP) based on the generalized extreme value distribution. The relative performance of t

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8

Morris, Brett M., Monica G. Bobra, Eric Agol, Yu Jin Lee, and Suzanne L. Hawley. "The stellar variability noise floor for transiting exoplanet photometry with PLATO." Monthly Notices of the Royal Astronomical Society 493, no. 4 (2020): 5489–98. http://dx.doi.org/10.1093/mnras/staa618.

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ABSTRACT One of the main science motivations for the ESA PLAnetary Transit and Oscillations (PLATO) mission is to measure exoplanet transit radii with 3 per cent precision. In addition to flares and starspots, stellar oscillations and granulation will enforce fundamental noise floors for transiting exoplanet radius measurements. We simulate light curves of Earth-sized exoplanets transiting continuum intensity images of the Sun taken by the Helioseismic and Magnetic Imager (HMI) instrument aboard the Solar Dynamics Observatory (SDO) to investigate the uncertainties introduced on the exoplanet r

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Wang, Gavin, and Néstor Espinoza. "A Blind Search for Transit Depth Variability with TESS." Astronomical Journal 167, no. 1 (2023): 1. http://dx.doi.org/10.3847/1538-3881/ad09bd.

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Abstract The phenomenon of transit depth variability offers a pathway through which processes such as exoplanet atmospheric activity and orbital dynamics can be studied. In this work we conduct a blind search for transit depth variations among 330 known planets observed by the Transiting Exoplanet Survey Satellite within its first four years of operation. Through an automated periodogram analysis, we identify four targets (KELT-8b, HAT-P-7b, HIP 65 Ab, and TrES-3b) that appear to show significant transit depth variability. We find that KELT-8b’s transit depth variability likely comes from cont

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10

Zhang, Michael, P. Wilson Cauley, Heather A. Knutson, et al. "More Evidence for Variable Helium Absorption from HD 189733b." Astronomical Journal 164, no. 6 (2022): 237. http://dx.doi.org/10.3847/1538-3881/ac9675.

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Abstract We present a new Keck/NIRSPEC observation of metastable helium absorption from the upper atmosphere of HD 189733b, a hot Jupiter orbiting a nearby moderately active star. We measure an average helium transit depth of 0.420% ± 0.013% integrated over the [−20, 20] km s−1 velocity range. Comparing this measurement to eight previously published transit observations with different instruments, we find that our depth is 32% (9σ) lower than the average of the three CARMENES transits, but only 16% (4.4σ) lower than the average of the five GIANO transits. We perform 1D hydrodynamical simulatio

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11

Dong, Kailing. "Analysis of Urban Rail Transit Station Planning Combining Simulated Annealing Algorithm." Discrete Dynamics in Nature and Society 2022 (March 7, 2022): 1–8. http://dx.doi.org/10.1155/2022/3941554.

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As a crucial node in the network system of urban transportation infrastructure, the consistent planning of the urban rail transit stations scientifically and reasonably is of highly significant importance to have a thorough understanding of the functional area division of a city and assess the improvement of facilities correlated with the rail transit infrastructure. In this study, the simulated annealing algorithm (SAA) is applied to the data analysis of the rail transit stations in a city. The method for the analysis of the urban rail transit stations combined with the SAA can achieve the di

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Lobodenko, M., Ya V. Pavlenko, I. Kulyk, A. Nahurna, M. Solomakha, and O. Baransky. "COMPARATIVE ANALYSIS OF OBSERVATIONS OF THE SELECTED EXOPLANET TRANSITS OBTAINED AT THE KYIV COMET STATION WITH THE DATABASE OF THE ORBITAL TELESCOPES TESS AND KEPLER." Odessa Astronomical Publications 35 (December 14, 2022): 44–49. http://dx.doi.org/10.18524/1810-4215.2022.35.268007.

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We present a comparative analysis of observations of the selected exoplanet transits obtained at the Kyiv Comet station with the database of the TESS (Transiting Exoplanet Survey Satellite) and Kepler space telescopes. The light curves obtained by the TESS and Kepler orbital telescopes were processed using a program based on the Python package Lightcurve 2.3v which is freely available in the MUST archive (Barbara A. Mikulski Archive for Space Telescopes). The ground based observations were carried out with the 70-cm telescope AZT- 8 (Lisnyky). Photometric processing of the ground based observa

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13

Ridden-Harper, A. R., C. U. Keller, M. Min, R. van Lieshout, and I. A. G. Snellen. "Chromatic transit light curves of disintegrating rocky planets." Astronomy & Astrophysics 618 (October 2018): A97. http://dx.doi.org/10.1051/0004-6361/201731947.

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Context. Kepler observations have revealed a class of short-period exoplanets, of which Kepler-1520 b is the prototype, which have comet-like dust tails thought to be the result of small, rocky planets losing mass. The shape and chromaticity of the transits constrain the properties of the dust particles originating from the planet’s surface, offering a unique opportunity to probe the composition and geophysics of rocky exoplanets. Aims. We aim to approximate the average Kepler long-cadence light curve of Kepler-1520 b and investigate how the optical thickness and transit cross section of a gen

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14

Heng, Kevin. "On physical interpretations of the reference transit radius of gas-giant exoplanets." Monthly Notices of the Royal Astronomical Society 490, no. 3 (2019): 3378–83. http://dx.doi.org/10.1093/mnras/stz2746.

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ABSTRACT Two theoretical quandaries involving transmission spectra of gas-giant exoplanets are elucidated. When computing the transit radius as a function of wavelength, one needs to specify a reference transit radius corresponding to a reference pressure. Mathematically, the reference transit radius is a constant of integration that originates from evaluating an integral for the transit depth. Physically, its interpretation has been debated in the literature. Jordán & Espinoza suggested that the optical depth is discontinuous across, and infinite below, the reference transit radius. Bétré

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Biersteker, John, and Hilke Schlichting. "Determining Exoplanetary Oblateness Using Transit Depth Variations." Astronomical Journal 154, no. 4 (2017): 164. http://dx.doi.org/10.3847/1538-3881/aa88c2.

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16

Petrucci, Romina, Emiliano Jofré, Martín Schwartz, Andrea Buccino, and Pablo Mauas. "TTVs study in southern stars." Proceedings of the International Astronomical Union 7, S286 (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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17

Kjurkchieva, Diana, Nikola Petrov, Sunay Ibryamov, Grigor Nikolov, and Velimir Popov. "New observations and transit solutions of the exoplanets HAT-P-53b and XO-5b." Serbian Astronomical Journal, no. 196 (2018): 15–20. http://dx.doi.org/10.2298/saj1896015k.

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We present photometric observations of transiting exoplanets HATP-53b and XO-5b by the Rozhen 2 m telescope. The modeling of the HAT-P-53b transit required bigger planet radius than the previously published value due to the bigger depth of the newly-observed transit. The transit solution of XO-5b led to values of fitted parameters within errors of the previously published results. Based on a time span of around 9 years we improved the orbital period of XO-5b to the value of 4.187751515 d. The quality of our data does not allow determination of planet temperatures by the transit solutions. Our

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18

Twicken, Joseph D., Jon M. Jenkins, Douglas A. Caldwell, et al. "TESS Science Processing Operations Center Photometric Precision Archival Product." Research Notes of the AAS 9, no. 6 (2025): 132. https://doi.org/10.3847/2515-5172/addec4.

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Abstract We report the delivery to the Mikulski Archive for Space Telescopes (MAST) of tables containing rms Combined Differential Photometric Precision (CDPP) values for all TESS 2 minutes cadence targets with Science Processing Operations Center (SPOC) light curves in Sectors 1–90. Each comma-separated values file contains CDPP values for all 2 minutes light curves in the given sector. The tables include robust rms CDPP values for the 15 trial transit pulse durations searched in the SPOC 2 minutes processing pipeline, ranging from 0.5 to 15.0 hr. For each pulse duration, CDPP is computed in

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Burdanov, A. Y., S. M. Lederer, M. Gillon, et al. "Ground-based follow-up observations of TRAPPIST-1 transits in the near-infrared." Monthly Notices of the Royal Astronomical Society 487, no. 2 (2019): 1634–52. http://dx.doi.org/10.1093/mnras/stz1375.

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Abstract The TRAPPIST-1 planetary system is a favourable target for the atmospheric characterization of temperate earth-sized exoplanets by means of transmission spectroscopy with the forthcoming James Webb Space Telescope (JWST). A possible obstacle to this technique could come from the photospheric heterogeneity of the host star that could affect planetary signatures in the transit transmission spectra. To constrain further this possibility, we gathered an extensive photometric data set of 25 TRAPPIST-1 transits observed in the near-IR J band (1.2 μm) with the UKIRT and the AAT, and in the N

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Tamburo, Patrick, Philip S. Muirhead, Allison M. McCarthy, et al. "The Perkins INfrared Exosatellite Survey (PINES). II. Transit Candidates and Implications for Planet Occurrence around L and T Dwarfs." Astronomical Journal 164, no. 6 (2022): 252. http://dx.doi.org/10.3847/1538-3881/ac9a52.

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Abstract We describe a new transit-detection algorithm designed to detect single-transit events in discontinuous Perkins INfrared Exosatellite Survey (PINES) observations of L and T dwarfs. We use this algorithm to search for transits in 131 PINES light curves and identify two transit candidates: 2MASS J18212815+1414010 (2MASS J1821+1414) and 2MASS J08350622+1953050 (2MASS J0835+1953). We disfavor 2MASS J1821+1414 as a genuine transit candidate due to the known variability properties of the source. We cannot rule out the planetary nature of 2MASS J0835+1953's candidate event and perform follow

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Padjaroen, T., S. Awiphan, and S. Komonjinda. "Transmission spectroscopy analyses of Jovian planets with Hubble Space Telescope." Journal of Physics: Conference Series 2653, no. 1 (2023): 012025. http://dx.doi.org/10.1088/1742-6596/2653/1/012025.

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Abstract Studying the chemical compositions of exoplanetary atmospheres provides valuable information about the conditions and characteristics of those atmospheres, which could help search for signs of extraterrestrial life. To date, over 3,000 exoplanets have been discovered using the transit method. The transmission spectroscopy technique, which studies exoplanetary atmospheres during their transits, is widely used to study the atmosphere of transiting exoplanets. Wide Field Camera 3 (WFC3), an instrument on the Hubble Space Telescope (HST), use the transmission spectroscopy technique by obs

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Ducrot, E., M. Gillon, L. Delrez, et al. "TRAPPIST-1: Global results of the Spitzer Exploration Science Program Red Worlds." Astronomy & Astrophysics 640 (August 2020): A112. http://dx.doi.org/10.1051/0004-6361/201937392.

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Context. With more than 1000 h of observation from Feb. 2016 to Oct. 2019, the Spitzer Exploration Program Red Worlds (ID: 13067, 13175 and 14223) exclusively targeted TRAPPIST-1, a nearby (12 pc) ultracool dwarf star, finding that it is orbited by seven transiting Earth-sized planets. At least three of these planets orbit within the classical habitable zone of the star, and all of them are well-suited for a detailed atmospheric characterization with the upcoming JWST. Aims. The main goals of the Spitzer Red Worlds program were (1) to explore the system for new transiting planets, (2) to inten

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Sulis, S., M. Lendl, S. Hofmeister, et al. "Mitigating flicker noise in high-precision photometry." Astronomy & Astrophysics 636 (April 2020): A70. http://dx.doi.org/10.1051/0004-6361/201937412.

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Context. In photometry, the short-timescale stellar variability (“flicker”), such as that caused by granulation and solar-like oscillations, can reach amplitudes comparable to the transit depth of Earth-sized planets and is correlated over the typical transit timescales. It can introduce systematic errors on the inferred planetary parameters when a small number of transits are observed. Aims. The objective of this paper is to characterize the statistical properties of the flicker noise and quantify its impact on the inferred transit parameters. Methods. We used the extensive solar observations

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Wood, Patricia L., and Pierre F. L. Maxted. "Transmission spectroscopy of the sodium doublet in WASP-17b with the VLT." Proceedings of the International Astronomical Union 6, S276 (2010): 491–92. http://dx.doi.org/10.1017/s174392131102093x.

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AbstractThe detection of sodium absorption during primary transit implies the presence of an atmosphere around an extrasolar planet. WASP-17b (Anderson et al. 2010a) is the least dense known planet, with a radius twice that of Jupiter. It orbits an F6-type star, and its low gravity gives its atmosphere a very large scale height. The sodium transit depth is expected to be 4.1 – 5.2 times deeper than for HD 209458b (Seager & Sasselov 2000). We obtained 24 spectra with the GIRAFFE spectrograph on the VLT, 8 during transit. We measured the flux in the sodium doublet at 5889.95 Å and 5895.92 Å

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Wong, Ian, Avi Shporer, Shreyas Vissapragada, et al. "TESS Revisits WASP-12: Updated Orbital Decay Rate and Constraints on Atmospheric Variability." Astronomical Journal 163, no. 4 (2022): 175. http://dx.doi.org/10.3847/1538-3881/ac5680.

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Abstract After observing WASP-12 in the second year of the primary mission, the Transiting Exoplanet Survey Satellite (TESS) revisited the system in late 2021 during its extended mission. In this paper, we incorporate the new TESS photometry into a reanalysis of the transits, secondary eclipses, and phase curve. We also present a new K s -band occultation observation of WASP-12b obtained with the Palomar/Wide-field Infrared Camera instrument. The latest TESS photometry spans three consecutive months, quadrupling the total length of the TESS WASP-12 light curve and extending the overall time ba

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Ding, Feng, Zheng Ma, Bing Zheng, et al. "Development and application of a refined port bathymetry model based on the FVCOM model." Journal of Physics: Conference Series 3007, no. 1 (2025): 012026. https://doi.org/10.1088/1742-6596/3007/1/012026.

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Abstract Safety is the foremost prerequisite for shipping, and refined port bathymetry services are a key factor in ensuring navigational safety. However, the issue of inconsistent and discontinuous vertical datums between different sea areas and adjacent ports has long been a critical challenge in bathymetric surveys. In this paper, a high-precision tidal model was established using the Finite Volume Coastal Ocean Model (FVCOM). We used harmonic analysis to calculate the depth datum for each grid point and combined these with nautical chart depths to construct a bathymetric model based on a c

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McKee, Brendan J., and Benjamin T. Montet. "Transit Depth Variations Reveal TOI-216 b to be a Super-puff." Astronomical Journal 165, no. 6 (2023): 236. http://dx.doi.org/10.3847/1538-3881/accd66.

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Abstract The planets of the TOI-216 system have been previously observed to exhibit large transit-timing variations, which enabled precise mass characterization of both transiting planets. In the first year of TESS observations, TOI-216 b exhibited grazing transits, precluding a measurement of its radius. In new observations, we demonstrate the orbit of the planet has precessed and it is now fully transiting, so we can accurately measure its radius. TOI-216 b is a puffy Neptune-mass planet, with a much larger radius that is now well constrained to 7.84 − 0.19 + 0.21 R ⊕ and a density of 0.201

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Sreejith, A. G., Kevin France, Luca Fossati, et al. "CUTE Reveals Escaping Metals in the Upper Atmosphere of the Ultrahot Jupiter WASP-189b." Astrophysical Journal Letters 954, no. 1 (2023): L23. http://dx.doi.org/10.3847/2041-8213/acef1c.

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Abstract Ultraviolet observations of ultrahot Jupiters, exoplanets with temperatures over 2000 K, provide us with an opportunity to investigate if and how atmospheric escape shapes their upper atmosphere. Near-ultraviolet transit spectroscopy offers a unique tool to study this process owing to the presence of strong metal lines and a bright photospheric continuum as the light source against which the absorbing gas is observed. WASP-189b is one of the hottest planets discovered to date, with a dayside temperature of about 3400 K orbiting a bright A-type star. We present the first near-ultraviol

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Guilluy, G., V. Andretta, F. Borsa, et al. "The GAPS programme at TNG." Astronomy & Astrophysics 639 (July 2020): A49. http://dx.doi.org/10.1051/0004-6361/202037644.

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Context. Exoplanets orbiting very close to their parent star are strongly irradiated. This can lead the upper atmospheric layers to expand and evaporate into space. The metastable helium (He I) triplet at 1083.3 nm has recently been shown to be a powerful diagnostic to probe extended and escaping exoplanetary atmospheres. Aims. We perform high-resolution transmission spectroscopy of the transiting hot Jupiter HD 189733 b with the GIARPS (GIANO-B + HARPS-N) observing mode of the Telescopio Nazionale Galileo, taking advantage of the simultaneous optical+near infrared spectral coverage to detect

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Silva-Válio, Adriana. "The influence of starspots activity on the determination of planetary transit parameters." Proceedings of the International Astronomical Union 5, S264 (2009): 440–42. http://dx.doi.org/10.1017/s1743921309993061.

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AbstractAs a planet eclipses its parent star, dark spots on the surface of the star may be occulted, causing a detectable variation in the transit light curve. There are basically two effects caused by the presence of spots on the surface of the star which can alter the shape of the light curve during transits and thus preclude the correct determination of the planet physical and orbital parameters. The first one is that the presence of many spots within the latitude band occulted by the planet will cause the depth of the transit in the light curve to be shallower. This will erroneously result

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Agol, Eric, Nicolas B. Cowan, James Bushong, et al. "Transits and secondary eclipses of HD 189733 with Spitzer." Proceedings of the International Astronomical Union 4, S253 (2008): 209–15. http://dx.doi.org/10.1017/s1743921308026422.

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AbstractWe present limits on transit timing variations and secondary eclipse depth variations at 8 microns with the Spitzer Space Telescope IRAC camera. Due to the weak limb darkening in the infrared and uninterrupted observing, Spitzer provides the highest accuracy transit times for this bright system, in principle providing sensitivity to secondary planets of Mars mass in resonant orbits. Finally, the transit data provides tighter constraints on the wavelength-dependent atmospheric absorption by the planet.

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Yoh, Allison C., Peter J. Haas, and Brian D. Taylor. "Understanding Transit Ridership Growth: Case Studies of Successful Transit Systems in the 1990s." Transportation Research Record: Journal of the Transportation Research Board 1835, no. 1 (2003): 111–20. http://dx.doi.org/10.3141/1835-14.

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During the economic boom of the late 1990s, transit ridership increased nationwide, but not all transit systems added riders in equal proportions. To examine agencies that were especially successful at increasing patronage during the late 1990s, in-depth, open-ended interviews were conducted with managers from 12 agencies that substantially increased ridership between 1995 and 1999. The transit agency managers reported a wide variety of factors that they believe influenced patronage on their systems. While it was initially hypothesized that transit managers would tend to cite factors internal

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Barmentloo, S., C. Dik, M. A. Kenworthy, et al. "A search for transiting companions in the J1407 (V1400 Cen) system." Astronomy & Astrophysics 652 (August 2021): A117. http://dx.doi.org/10.1051/0004-6361/202140768.

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Context. In 2007, the young star 1SWASP J140747.93-394 542.6 (V1400 Cen) underwent a complex series of deep eclipses over 56 days. This was attributed to the transit of a ring system filling a large fraction of the Hill sphere of an unseen substellar companion. Subsequent photometric monitoring has not found any other deep transits from this candidate ring system, but if there are more substellar companions and if they are coplanar with the potential ring system, there is a chance that they will transit the star as well. This young star is active, and the light curves show a 5% modulation in a

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Lo, Tinfei, and Jiani Fu. "Analysis of Eclipsing Binary Stars and Identification of Exoplanets Using Transit Timing Variation Using data from TESS." Journal of Physics: Conference Series 2381, no. 1 (2022): 012106. http://dx.doi.org/10.1088/1742-6596/2381/1/012106.

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Abstract This study uses openly available TESS (Transiting Exoplanet Sky Survey) data to detect evidence for potential exoplanet transits in an eclipsing binary system. Using the Python transit light curve analysis package lightcurve, we discuss the characteristics of an eclipsing binary star’s light curve in determining the classification of a system. In addition, we also study phenomena on a light curve that indicates the existence of a potential exoplanet. Although this investigation yields null results and finds no conclusive evidence, suggesting the presence of exoplanet transits in known

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Kanodia, Shubham, Suvrath Mahadevan, Jessica Libby-Roberts, et al. "TOI-5205b: A Short-period Jovian Planet Transiting a Mid-M Dwarf." Astronomical Journal 165, no. 3 (2023): 120. http://dx.doi.org/10.3847/1538-3881/acabce.

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Abstract We present the discovery of TOI-5205b, a transiting Jovian planet orbiting a solar metallicity M4V star, which was discovered using Transiting Exoplanet Survey Satellite photometry and then confirmed using a combination of precise radial velocities, ground-based photometry, spectra, and speckle imaging. TOI-5205b has one of the highest mass ratios for M-dwarf planets, with a mass ratio of almost 0.3%, as it orbits a host star that is just 0.392 ± 0.015 M ⊙. Its planetary radius is 1.03 ± 0.03 R J, while the mass is 1.08 ± 0.06 M J. Additionally, the large size of the planet orbiting a

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Xia, Xian Peng, Jing Liu, Hai Yu Li, Hong Hui Dong, Yi Fan Gao, and Ming Chao Wu. "High Reliability Wireless Coverage Technology Solution to Rail Transit Train-Ground Communication." Applied Mechanics and Materials 513-517 (February 2014): 709–12. http://dx.doi.org/10.4028/www.scientific.net/amm.513-517.709.

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With the development of science and technology and urbanization process in depth, rail transit plays a more and more important role in the city. Train-ground communication is an important part of the safe operation of the rail transit trains. According to the traits of wireless train-ground communication, this paper proposes a high reliability wireless coverage technology solution to rail transit communication. Then this paper introduces the implementation process of the solution and verifies the wireless coverage range in this solution.

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Parviainen, H., E. Palle, M. R. Zapatero-Osorio, et al. "MuSCAT2 multicolour validation of TESS candidates: an ultra-short-period substellar object around an M dwarf." Astronomy & Astrophysics 633 (January 2020): A28. http://dx.doi.org/10.1051/0004-6361/201935958.

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Context. We report the discovery of TOI 263.01 (TIC 120916706), a transiting substellar object (R = 0.87 RJup) orbiting a faint M3.5 V dwarf (V = 18.97) on a 0.56 d orbit. Aims. We setout to determine the nature of the Transiting Exoplanet Survey Satellite (TESS) planet candidate TOI 263.01 using ground-based multicolour transit photometry. The host star is faint, which makes radial-velocity confirmation challenging, but the large transit depth makes the candidate suitable for validation through multicolour photometry. Methods. Our analysis combines three transits observed simultaneously in r′

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Hazra, Gopal, Aline A. Vidotto, Stephen Carolan, Carolina Villarreal D’Angelo, and Ward Manchester. "The impact of coronal mass ejections and flares on the atmosphere of the hot Jupiter HD189733b." Monthly Notices of the Royal Astronomical Society 509, no. 4 (2021): 5858–71. http://dx.doi.org/10.1093/mnras/stab3271.

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ABSTRACT High-energy stellar irradiation can photoevaporate planetary atmospheres, which can be observed in spectroscopic transits of hydrogen lines. For the exoplanet HD189733b, multiple observations in the Ly α line have shown that atmospheric evaporation is variable, going from undetected to enhanced evaporation in a 1.5-yr interval. Coincidentally or not, when HD189733b was observed to be evaporating, a stellar flare had just occurred 8 h prior to the observation. This led to the question of whether this temporal variation in evaporation occurred due to the flare, an unseen associated coro

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Goch, Katarzyna, Szymon Ochota, Monika Piotrkowska, and Zuzanna Kunert. "Measuring dynamic public transit accessibility to local centres in Warsaw." Urban Development Issues 58, no. 1 (2018): 29–40. http://dx.doi.org/10.2478/udi-2018-0021.

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Abstract Over the last decade the number of studies on public transit accessibility has significantly increased. The aim of the study was to analyse the scope of application of measurements of the dynamic time accessibility in transportation systems for evaluation purposes. It was assumed that the indicator is a feasible measure for basic analysis however additional indicators are needed for reliable assessment. The study included assessing access to the global centre of Warsaw and to local and district centres in particular units. Public transit accessibility was analysed using schedule-based

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Juvan, Ines G., M. Lendl, P. E. Cubillos, et al. "PyTranSpot: A tool for multiband light curve modeling of planetary transits and stellar spots." Astronomy & Astrophysics 610 (February 2018): A15. http://dx.doi.org/10.1051/0004-6361/201731345.

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Several studies have shown that stellar activity features, such as occulted and non-occulted starspots, can affect the measurement of transit parameters biasing studies of transit timing variations and transmission spectra. We present PyTranSpot, which we designed to model multiband transit light curves showing starspot anomalies, inferring both transit and spot parameters. The code follows a pixellation approach to model the star with its corresponding limb darkening, spots, and transiting planet on a two dimensional Cartesian coordinate grid. We combine PyTranSpot with a Markov chain Monte C

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Raetz, St, G. Maciejewski, M. Mugrauer, et al. "Transit timing, depth, and duration variation in exoplanet TrES-2?" EPJ Web of Conferences 11 (2011): 05007. http://dx.doi.org/10.1051/epjconf/20101105007.

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Raetz, St, G. Maciejewski, M. Mugrauer, et al. "Transit timing, depth, and duration variation in exoplanet TrES-2?" EPJ Web of Conferences 11 (2011): 05007. http://dx.doi.org/10.1051/epjconf/20111105007.

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Scully, Brandan M., and Kenneth Ned Mitchell. "Underkeel Clearance Reliability Model for Dredged Navigation Channels." Transportation Research Record: Journal of the Transportation Research Board 2611, no. 1 (2017): 41–49. http://dx.doi.org/10.3141/2611-05.

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This paper presents a reliability measure for selecting marine navigation channel maintenance depth. Resource constraints have resulted in dredging requirements outpacing the funds available to the U.S. Army Corps of Engineers to perform navigation channel maintenance dredging, but navigation managers lack a method to objectively select maintenance depth alternatives to authorized project depths. The reliability of a navigation channel can be determined as the probability that a vessel's net underkeel clearance is greater than or equal to 0. Net underkeel clearance was hindcast from underkeel

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Fall, Madièye, Déthié Sarr, Hamed FALL, and Oustasse Abdoulaye Sall. "Numerical Modelling of the Evolution of Sedimentary and Topo-Bathymetric Transit Rates: The Case of the Beaches of Rufisque on the Small Senegalese Coast." International Journal of Research and Review 12, no. 4 (2025): 368–74. https://doi.org/10.52403/ijrr.20250444.

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This study seeks to estimate by a numerical approach the average rate of sediment transit along the sandy beaches of Rufisque on the small Senegalese coast, and to study its longitudinal variability as a function of this beach. The transit estimation approach is based on the long-term analysis, between 1985 and 2021, of the topo-bathymetric evolution of the seabed. By using remote sensing methods and Geographic Information Systems, the quality of the bathymetric data allows the implementation, and during each period, of a Digital Depth Model (DEM). The superposition of two Numerical Depth Mode

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Alderson, Lili, Natasha E. Batalha, Hannah R. Wakeford, et al. "JWST COMPASS: NIRSpec/G395H Transmission Observations of the Super-Earth TOI-836b." Astronomical Journal 167, no. 5 (2024): 216. http://dx.doi.org/10.3847/1538-3881/ad32c9.

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Abstract We present two transit observations of the ∼870 K, 1.7 R ⊕ super-Earth TOI-836b with JWST NIRSpec/G395H, resulting in a 2.8–5.2 μm transmission spectrum. Using two different reduction pipelines, we obtain a median transit depth precision of 34 ppm for Visit 1 and 36 ppm for Visit 2, leading to a combined precision of 25 ppm in spectroscopic channels 30 pixels wide (∼0.02 μm). We find that the transmission spectrum from both visits is well fit by a zero-sloped line, by fitting zero-sloped and sloped lines as well as step functions to our data. Combining both visits, we are able to rule

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Mitani, Hiroto, Riouhei Nakatani, and Naoki Yoshida. "Stellar activity effects on the atmospheric escape of hot Jupiters." Proceedings of the International Astronomical Union 16, S362 (2020): 158–63. http://dx.doi.org/10.1017/s1743921322001260.

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AbstractTransit observations have revealed the existence of atmospheric escape in several hot Jupiters. High energy photons from the host star heat the upper atmosphere and drive the hydrodynamic escape. The escaping atmosphere can interact with the stellar wind from the host star. We run radiation hydrodynamics simulations with non-equilibrium chemistry to investigate the wind effects on the escape and the transit signature. Our simulations follow the planetary outflow driven by the photoionization heating and the wind interaction in a dynamically coupled, self-consistent manner. We show that

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Murgas, F., G. Chen, L. Nortmann, E. Palle, and G. Nowak. "The GTC exoplanet transit spectroscopy survey." Astronomy & Astrophysics 641 (September 2020): A158. http://dx.doi.org/10.1051/0004-6361/202038161.

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Context. One of the main atmospheric features in exoplanet atmospheres, detectable both from ground- and space-based facilities, is Rayleigh scattering. In hydrogen-dominated planetary atmospheres, Rayleigh scattering causes the measured planetary radius to increase toward blue wavelengths in the optical range. Aims. We aim to detect and improve our understanding of several features in the optical range observable in planetary atmospheres. We focus on studying transiting exoplanets that present a wide range of orbital periods, masses, radii, and irradiation from their host star. Methods. We ob

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Tusay, Nick, Jason T. Wright, Thomas G. Beatty, et al. "A Disintegrating Rocky World Shrouded in Dust and Gas: Mid-infrared Observations of K2-22 b Using JWST." Astrophysical Journal Letters 987, no. 1 (2025): L6. https://doi.org/10.3847/2041-8213/addfd0.

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Abstract The disintegrating ultrashort period rocky exoplanet K2-22 b periodically emits dusty clouds in a dynamically chaotic process resulting in a variable transit depth from 0% to 1.3%. The effluents that sublimate off the surface and condense out in space are probably representative of the formerly interior layers convectively transported to the molten surface. Transmission spectroscopy of these transiting clouds reveals spectral fingerprints of the interior composition of this rocky world. We used JWST’s Mid-Infrared Instrument as a low-resolution slitless spectrograph to observe four pr

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Saito, Roberto, Paulo Henrique Silva, Antonio Kanaan, William Schoenell, Luciano Fraga, and Albert Bruch. "Observing exoplanets from Brazil: the first try." Proceedings of the International Astronomical Union 4, S253 (2008): 454–55. http://dx.doi.org/10.1017/s1743921308026914.

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AbstractThis project consists in mapping a 4-square-degree region searching for exoplanets using the transit method. This “mini-survey” will be the first use of the 16″ robotic telescope developed by Universidade Federal de Santa Catarina (UFSC-Brazil) and Laboratório Nacional de Astrofísica (LNA/MCT-Brazil). The chosen region is over the Columba constellation and our first observations have shown that we have enough signal-to-noise ratio to search for transits on about 20,000 stars with ~13 < I < 16 mag, a magnitude range between the OGLE and HAT projects. In this star sample we expect

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Yang, Kang, LixiaWang, Ge Jiawei, and Wang Xuefeng. "Study on the Pricing and Path Scheme Comparison of Transit Freight." International Journal of Engineering and Management Research 8, no. 6 (2018): 55–68. https://doi.org/10.31033/ijemr.8.6.6.

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This paper aims to optimize the transportation network and transportation organization strategy of Transport through China, enabling operators to obtain greater profits, improving the efficiency of transit freight transport, and solving the problem of transportation pricing and route selection of transit goods. In this paper, the growth trend of transit transport demand is firstly determined. On this basis, the ultimate goal is to maximize the transport profit of the operator. In-depth analysis is made from the perspectives of transport income and transport cost. In addition, through combing e

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