Astronomers have been scanning hundreds of stars for “anomalous transits

A transit is when a planet passes in front of its star, slightly dimming the star’s light. This dimming can be seen in light curves, which are graphs that show light received over time

Astronomers have developed an algorithm to search for anomalous transits in stellar lightcurves. The algorithm reported results for 218 confirmed transiting exoplanet systems from Kepler. 

Astronomers also occasionally detect objects with unexpected shapes, unexplainable photometry, or unprecedented spectra. However, many of these anomalies are discarded as noise, contamination, or faulty analysis.

Telescopes have been collecting copious amounts of data on exoplanets in recent years. One of the most common datasets tracks what are known as “transits,” where an exoplanet crosses in front of its host star and dims the star’s light slightly as it does so

The transit photometry method has several drawbacks: 

• Not all planets transit Only a small proportion of distant planets orbit their star in a straight line of sight with Earth. The planet must pass directly between its star and Earth. 
• Only detects large planets From the ground, the transit method can only detect very large and gaseous planets. To detect Earth-like “rocky” exoplanets, astronomers need to go to space. 
• Low probability Transits are unlikely to appear in randomly oriented planet systems. 
• False positives Astrophysical phenomena can mimic transits and lead to false detection positives. For example, a drop in a star’s brightness could be due to another object passing in front of the star. Binary star systems produce similar light curves, with a random probability of finding a false positive of 300/190,000. 

The transit method’s main advantage is that it can determine the size of the planet from the light curve. When combined with the radial-velocity method, which determines the planet’s mass, astronomers can determine the planet’s density

The transit method is one of the most effective and sensitive methods for detecting extrasolar planets. It’s especially advantageous for space-based observatories that can continuously observe stars for weeks or months

The transit method works best for planets that orbit very close to their host star. Most exoplanets have been discovered using this method. 

The transit method is also advantageous because it can provide accurate constraints on the size of detected planets. This is based on the extent to which a star’s light curve changes as a result of a transit. 

When combined with the radial-velocity method, which determines the planet’s mass, astronomers can determine the density of the planet, and hence learn something about the planet’s physical structure.

Transits of exoplanets can provide valuable information about the planet’s properties and potential habitability. 

Here are some properties that can be determined from transits: 

• Size The depth of the dip in brightness during a transit can be used to determine the planet’s size. 
• Orbital distance The duration of the dip can be used to determine the planet’s orbital distance. 
• Atmosphere The sharpness of the dip can indicate if the planet has a significant atmosphere. Under certain conditions, the content of the atmosphere can be measured by using a spectroscope. 
• Albedo The planet’s size and orbital distance can be used to determine its albedo. 
• Surface temperature Information about the planet’s surface temperature can be obtained from planets that transit. 

The transit method can also provide information about the planet’s mass and density, which can help determine its composition and potential habitability.

For planets that do transit, astronomers can get valuable information about the planet’s atmosphere, surface temperatures and size. For most sun-like stars, an orbiting planet even as large as a brown dwarf will only cause an observed reduction in brightness of the star of a few percent or less during a transit

Astronomers occasionally detect objects with unexpected shapes, unexplainable photometry, or unprecedented spectra. These anomalies are inconsistent with our current knowledge of the universe

Astronomers say they’re likely to discover natural explanations for these anomalies. Some examples of strange, unexplained objects include: 

• “Puffy” planets 
• Slow-spinning pulsars 
• Interstellar asteroids 
• Fast radio bursts from beyond the Milky Way 

Photometry is a technique that measures the brightness of a star in an image. 

Some of these anomalies are discarded as mere noise, contamination, or faulty analysis.

Dec. 15, 2023 — A team of astronomers has used asteroseismology, or the study of stellar oscillations, to accurately measure the distance of stars from the Earth. Their research examined thousands of stars and checked the measurements taken during the Gaia mission

When an exoplanet crosses in front of its host star, it’s known as a transit. This event causes a slight dimming of the star’s light. 

The dimming is too small to see with the human eye. However, computers can compare a star’s brightness over time to detect the small changes in brightness during the exoplanet’s transit. 

The transit detection method is a popular method for finding exoplanets. By carefully monitoring these transits, scientists can determine the presence and characteristics of the exoplanet. 

The graph of the dip in brightness is called a light curve

The transit technique is also known as the transit method. 

Here are some other methods for detecting exoplanets: 

• Direct imaging Uses large telescopes with adaptive optics and coronagraphs to directly image the exoplanet. 
• Astrometry Measures the position and movement of a star to detect tiny changes in position as the star wobbles around the center of mass of the planetary system. 
• Gravitational microlensing Uses the gravity of the planet and star to focus light rays from the distant planet onto an observer. This effect only occurs when the two stars are almost exactly aligned. 
• Doppler spectroscopy Also known as the radial-velocity method, this indirect method uses radial-velocity measurements to find extrasolar planets and brown dwarfs.

Astronomers have developed an algorithm to search for anomalous transits in stellar lightcurves. The algorithm reported results for 218 confirmed transiting exoplanet systems from Kepler

A light curve is a graph of the light intensity of a celestial object or region as a function of time. Light curves can be periodic or aperiodic. The study of the light curve, together with other observations, can yield considerable information about the physical process that produces it. 

The Kepler space telescope has discovered over 2,800 confirmed exoplanets, which are planets orbiting stars outside our own solar system. The Kepler mission has detected bodies with a wide variety of properties, with significant ranges in orbital distances, masses, radii, composition, habitability, and host star type

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