NEAR-INFRARED THERMAL EMISSION DETECTIONS OF A NUMBER OF HOT JUPITERS AND THE SYSTEMATICS OF GROUND-BASED NEAR-INFRARED PHOTOMETRY

Allen et al. (1972) observed 40 WR stars in the |1.6µ| and |2.2µ| bands, and found evidence of interstellar dust emission in the WC9 stars Ve 2–45, AS320 and HD 313643. Hackwell et al. (1974) reported 2.3 to 23 µ photometry of 19 WR stars and concluded that the excess infrared radiation from the Wolf-Rayet stars (except for the WC9 stars) could be explained by free-free emission from a hot circumstellar shell. Gehrz and Hackwell (1974) found from 2.3 to 23 µ photometry that three out of four WC stars appear to be embedded in thick circumstellar dust (graphite) shells, and concluded that WC9 stars may form a distinct Wolf-Rayet class. Cohen et al. (1975) derived energy distributions of 23 Wolf-Rayet stars from 3µ-11µ scanner spectrophotometry and infrared photometry, and concluded that WN stars show only free-free emission whereas only WC stars show dust. The excesses in WC9 stars are interpreted as thermal emission by graphite grains.

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Lessons from detections of the near-infrared thermal emission of hot Jupiters

Proceedings of the International Astronomical Union ◽

10.1017/s1743921311020102 ◽

2010 ◽

Vol 6 (S276) ◽

pp. 154-157

Author(s):

Bryce Croll

Keyword(s):

Near Infrared ◽

Thermal Emission ◽

Temperature Inversion ◽

Infrared Emission ◽

Atmospheric Dynamics ◽

Mid Infrared ◽

Hot Jupiters ◽

Star Activity ◽

Near Infrared Emission

AbstractThere have recently been a flood of ground-based detections of the near-infrared thermal emission of a number of hot Jupiters. Although these near-infrared detections have revealed a great deal about the atmospheric characteristics of individual hot Jupiters, the question is: what information does this ensemble of near-infrared detections reveal about the atmospheric dynamics and reradiation of all hot Jupiters? I explore whether there is any correlation between how brightly these planets shine in the near-infrared compared to their incident stellar flux, as was theoretically predicted to be the case. Secondly, I look for whether there is any correlation between the host star's activity and the planet's near-infrared emission, like there is in the mid-infrared, where Spitzer observations have revealed a correlation between the host star activity with the presence, or lack thereof, of a temperature inversion and a hot stratosphere.

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Extending the Red Giant Branch versus Metallicity Calibration toward Metal-poor Systems: Near-Infrared Photometry of the Galactic Globular Clusters M56 and M15

The Astronomical Journal ◽

10.1086/301363 ◽

2000 ◽

Vol 119 (5) ◽

pp. 2274-2281 ◽

Cited By ~ 10

Author(s):

Valentin D. Ivanov ◽

Jordanka Borissova ◽

Almudena Alonso-Herrero ◽

Tatiana Russeva

Keyword(s):

Globular Clusters ◽

Near Infrared ◽

Infrared Photometry ◽

Galactic Globular Clusters ◽

Red Giant

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Shoreline Changes along Northern Ibaraki Coast after the Great East Japan Earthquake of 2011

Remote Sensing ◽

10.3390/rs13071399 ◽

2021 ◽

Vol 13 (7) ◽

pp. 1399

Author(s):

Quang Nguyen Hao ◽

Satoshi Takewaka

Keyword(s):

Near Infrared ◽

Thermal Emission ◽

Sandy Beaches ◽

Great East Japan Earthquake ◽

Shoreline Changes ◽

Run Up ◽

Tsunami Run Up ◽

Sentinel 2 ◽

Infrared Radiometer

In this study, we analyze the influence of the Great East Japan Earthquake, which occurred on 11 March 2011, on the shoreline of the northern Ibaraki Coast. After the earthquake, the area experienced subsidence of approximately 0.4 m. Shoreline changes at eight sandy beaches along the coast are estimated using various satellite images, including the ASTER (Advanced Spaceborne Thermal Emission and Reflection Radiometer), ALOS AVNIR-2 (Advanced Land Observing Satellite, Advanced Visible and Near-infrared Radiometer type 2), and Sentinel-2 (a multispectral sensor). Before the earthquake (for the period March 2001–January 2011), even though fluctuations in the shoreline position were observed, shorelines were quite stable, with the averaged change rates in the range of ±1.5 m/year. The shoreline suddenly retreated due to the earthquake by 20–40 m. Generally, the amount of retreat shows a strong correlation with the amount of land subsidence caused by the earthquake, and a moderate correlation with tsunami run-up height. The ground started to uplift gradually after the sudden subsidence, and shoreline positions advanced accordingly. The recovery speed of the beaches varied from +2.6 m/year to +6.6 m/year, depending on the beach conditions.

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