Barium produces emission lines at at least 21 different wavelengths in the visible range,
including at least one each in red, orange, yellow, green, blue, indigo, violet.
The visible spectrum wavelengths of Krypton fall in the range of approximately 440 to 740 nanometers. This corresponds to the blue to red part of the visible light spectrum.
It differs by that white light spectrum is continuous and consists of light of all wavelengths. Emission spectrum is not continuous. It consists of bright lines at specific wavelengths, with complete darkness between them.
Red, blue, green, and violet are found in the emission spectrum of hydrogen.
The spectrum of helium consists of distinct lines at specific wavelengths, known as emission lines, due to the transition of electrons between energy levels. In contrast, the spectrum of white light from the Sun is continuous, with all visible wavelengths present. The presence of absorption lines in the solar spectrum, caused by elements in the Sun's atmosphere absorbing specific wavelengths, further distinguishes it from the discrete emission lines of helium.
The emission spectrum of barium nitrate typically includes several bands of light in the visible region, with some lines in the blue-green part of the spectrum being the most prominent. The specific wavelengths and intensities of these lines can vary depending on the experimental conditions.
The difference between continuous spectrum and the atomic emission espectrum of an element is that in emission spectrum, only certain specific frequencies of light are emitted while in a continuous spectrum, a continuous range of colors are seen in the visible light.
The visible spectrum wavelengths of Krypton fall in the range of approximately 440 to 740 nanometers. This corresponds to the blue to red part of the visible light spectrum.
It differs by that white light spectrum is continuous and consists of light of all wavelengths. Emission spectrum is not continuous. It consists of bright lines at specific wavelengths, with complete darkness between them.
The emission of sodium lies in the yellow region
Red, blue, green, and violet are found in the emission spectrum of hydrogen.
The spectrum of helium consists of distinct lines at specific wavelengths, known as emission lines, due to the transition of electrons between energy levels. In contrast, the spectrum of white light from the Sun is continuous, with all visible wavelengths present. The presence of absorption lines in the solar spectrum, caused by elements in the Sun's atmosphere absorbing specific wavelengths, further distinguishes it from the discrete emission lines of helium.
The emission spectrum of barium nitrate typically includes several bands of light in the visible region, with some lines in the blue-green part of the spectrum being the most prominent. The specific wavelengths and intensities of these lines can vary depending on the experimental conditions.
Red.
Atomic emission spectra show specific wavelengths of light emitted by atoms when electrons transition from higher energy levels to lower ones. These spectra typically lie in the visible and ultraviolet regions of the electromagnetic spectrum.
An object appears a certain color because it reflects specific wavelengths in the visible spectrum while absorbing others. For example, a blue object reflects blue wavelengths and absorbs other colors.
The sun emits a range of wavelengths primarily in the visible, ultraviolet, and infrared regions. The peak of its emission is in the visible light spectrum, which is why we see the sun as a bright yellow/white. Green, blue, and violet light are also emitted, along with ultraviolet and infrared radiation.
The sun has 3 layers - the photosphere, the chromosphere, the corona. Photosphere is the visible surface and gives the absorption spectrum. Chromosphere is the pinkish discharge encircling the Sun, visible only during a total eclipse. This gives the emission spectrum. Corona is the halo encircling the chromosphere. THis gives the coronal spectrum.