Starlight

For other uses, seeStarlight (disambiguation).

Starry sky crossed with theMilky Wayand ameteor

Starlightis thelightemitted bystars.It typically refers tovisibleelectromagnetic radiationfrom stars other than theSun,observable fromEarthatnight,although a component of starlight is observable from Earth duringdaytime.

Sunlightis the term used for the Sun's starlight observed during daytime. During nighttime,albedodescribes solar reflections from otherSolar Systemobjects, includingmoonlight,planetshine,andzodiacal light.

Observation

Observation and measurement of starlight throughtelescopesis the basis for many fields ofastronomy,includingphotometryandstellar spectroscopy.Hipparchusdid not have a telescope or any instrument that could measure apparent brightness accurately, so he simply made estimates with his eyes. He sorted the stars into six brightness categories, which he called magnitudes.He referred to the brightest stars in his catalog as first-magnitude stars and those so faint he could barely see them as sixth-magnitude stars.

Starlight is also a notable part of personal experience and humanculture,impacting a diverse range of pursuits includingpoetry,astronomy,and military strategy.

TheUnited States Armyspent millions of dollars in the 1950s and onward to develop astarlight scope,that could amplify starlight, moonlight filtered by clouds, and thefluorescenceof rottingvegetationabout 50,000 times to allow a person to see in the night.In contrast to previously developed active infrared system such assniperscope,it was a passive device and did not require additional light emission to see.

The average color of starlight in theobservable universeis a shade of yellowish-white that has been given the nameCosmic Latte.

Starlight spectroscopy, examination of the stellar spectra, was pioneered byJoseph Fraunhoferin 1814.Starlight can be understood to be composed of three main spectra types,continuous spectrum,emission spectrum,andabsorption spectrum.

Starlight illuminance coincides with the human eye's minimum illuminance (~0.1mlx) while moonlight coincides with the human eye's minimum colour vision illuminance (~50 mlx).  

One of the oldest stars yet identified -  oldest but not most distant in this case - was identified in 2014: while "only" 6,000 light years away, the starSMSS J031300.36−670839.3was determined to be 13.8 billion years old, or more or less the sameage as the universeitself.The starlight shining on Earth includes this star.

Photography

Night photographyincludes photographing subjects that are lit primarily by starlight.Directly taking images of night sky is also a part ofastrophotography.Like other photography, it can be used for the pursuit of science and/or leisure.Subjects includenocturnal animals.In many cases starlight photography may also overlap with a need to understand the impact ofmoonlight.

Polarization

Starlight intensity has been observed to be a function of itspolarization.

Starlight becomes partiallylinearly polarizedby scattering from elongatedinterstellar dustgrains whose long axes tend to be oriented perpendicular to the galacticmagnetic field.According to theDavis–Greenstein mechanism,the grains spin rapidly with their rotation axis along the magnetic field. Light polarized along the direction of the magnetic fieldperpendicularto the line of sight is transmitted, while light polarized in the plane defined by the rotating grain is blocked. Thus the polarization direction can be used to map thegalactic magnetic field.The degree of polarization is on the order of 1.5% for stars at 1,000parsecs' distance.

Normally, a much smaller fraction ofcircular polarizationis found in starlight. Serkowski, Mathewson and Fordmeasured the polarization of 180 stars in UBVR filters. They found a maximum fractional circular polarization of$q=6\times 10^{-4}$,in the R filter.

The explanation is that the interstellar medium is optically thin. Starlight traveling through a kiloparsec column undergoes about a magnitude of extinction, so that the optical depth ~ 1. An optical depth of 1 corresponds to a mean free path, which is the distance, on average that a photon travels before scattering from a dust grain. So on average, a starlight photon is scattered from a single interstellar grain; multiple scattering (which produces circular polarization) is much less likely. Observationally,the linear polarization fraction p ~ 0.015 from a single scattering; circular polarization from multiple scattering goes as$p^{2}$,so we expect a circularly polarized fraction of$q\sim 2\times 10^{-4}$.

Light from early-type stars has very little intrinsic polarization. Kemp et al.measured the optical polarization of the Sun at sensitivity of$3\times 10^{-7}$;they found upper limits of$10^{-6}$for both$p$(fraction of linear polarization) and$q$(fraction of circular polarization).

The interstellar medium can produce circularly polarized (CP) light from unpolarized light by sequential scattering from elongated interstellar grains aligned in different directions. One possibility is twisted grain alignment along the line of sight due to variation in the galactic magnetic field; another is the line of sight passes through multiple clouds. For these mechanisms the maximum expected CP fraction is$q\sim p^{2}$,where$p$is the fraction of linearly polarized (LP) light. Kemp & Wolstencroftfound CP in six early-type stars (no intrinsic polarization), which they were able to attribute to the first mechanism mentioned above. In all cases,$q\sim 10^{-4}$in blue light.

Martinshowed that the interstellar medium can convert LP light to CP by scattering from partially aligned interstellar grains having a complex index of refraction. This effect was observed for light from theCrab Nebulaby Martin, Illing and Angel.

An optically thick circumstellar environment can potentially produce much larger CP than the interstellar medium. Martinsuggested that LP light can become CP near a star by multiple scattering in an optically thick asymmetric circumstellar dust cloud. This mechanism was invoked by Bastien, Robert and Nadeau,to explain the CP measured in 6 T-Tauri stars at a wavelength of 768 nm. They found a maximum CP of$q\sim 7\times 10^{-4}$.Serkowskimeasured CP of$q=7\times 10^{-3}$for the red supergiantNML Cygniand$q=2\times 10^{-3}$in the long-period variable M star VYCanis Majorisin the H band, ascribing the CP to multiple scattering incircumstellar envelopes.Chrysostomou et al.found CP with q of up to 0.17 in theOrionOMC-1 star-forming region, and explained it by reflection of starlight from aligned oblate grains in the dusty nebula.

Circular polarization of zodiacal light andMilky Waydiffuse galactic light was measured at wavelength of 550 nm by Wolstencroft and Kemp.They found values of$q\sim 5\times 10^{-3}$,which is higher than for ordinary stars, presumably because of multiple scattering from dust grains.

See also

• List of brightest stars
• Purkinje effect
• Sunlight
• Moonlight