#spectroscopy
JMW Turner’s Fishermen at Sea.
The traditional oil paints popular up to the 19th Century were made by grinding pigments with linseed, walnut or poppy seed oil – but while they produced stunning hues, their drying time meant that it could could take months or even years to complete a painting if several layers of colour were used.
Artists like JMW Turner understandably didn’t want to spend their lives watching paint dry, so they collaborated with chemists to produce gels that could be added to oil-based paints to shorten drying times.
Now, researchers at CNRS, UPMC and Collège de France have used spectroscopy to uncover the chemical secrets behind these gels.
The supramolecular structure of the gel is revealed by freeze fracture electron microscopy. Aa frozen specimen is fractured along natural planes, making an impression or replica of the exposed surface,then examined using transmission electron microscopy. Credit: LAMS (CNRS/UPMC)
They found that lead, in its acetate form, is essential to the formation of these gels. But other questions remained – how do they bind with the paint? How do they age?
The researchers reconstituted the original paint formulas and were able to reproduce the gels using lead and mastic to study their rheological properties, such as flow and deformation behaviour. They found that even minute amounts of the gels would modify the characteristics of the paint, yielding superior elastic properties.
On canvas, the consistency of gels and gel-paint mixtures differs greatly from that of paint alone, which spreads without retaining volume. Credit: Hélène Pasco, LAMS (CNRS, UPMC)
Using spectroscopic techniques, they defined the molecular interactions of the hybrid organic-inorganic gels and the mechanisms of the gelling process. They found that the lead not only catalysed the gelling process but contributed to the structure of the medium itself.
The challenge, now, is to understand how the lead binds with the resin and which conditions are best and worst for their conservation.
** This note was inspired from a comment on one of our previous post. Do check it out before you read this one.
The emission spectrum of atomic hydrogen is given by this amazing spectral series diagram:
Let’s take a closer look at only the visible portion of the spectrum i.e the Balmer series.
If a hydrogen lamp and a diffraction grating just happen to be with you, you can take a look at the hydrogen lamp through the diffraction grating, these lines are what you would see:
These are known emission lines and they occur when the hydrogen atoms in the lamp return to a state of lower energy from an excited energy state.
Representation of emission and absorption using the Bohr’s model
Here’s another scenario that could also happen:
You have a bright source of light with a continuous spectrum and in between the source and the screen, you introduce a gas (here, sodium)
Source: Harvard Natural sciences
The gas absorbs light at particular frequencies and therefore we get dark lines in the spectrum.
This is known as absorption line. The following diagram summarizes what was told thus-far in a single image:
The absorption and emission spectrum for hydrogen look like so :
Stars and Hydrogen
One of the comments from the previous post was to show raw spectrum data of what was being presented to get a better visual aid.
Therefore,the following spectrum is a spectrum of a star taken from the Sloan Digital Sky Survey (SDSS)
Plot of wavelength vs median-flux
Here’s the spectrum with all the absorption lines labelled:
You can clearly see the Balmer series of hydrogen beautifully encoded in this spectrum that was taken from a star that is light-years away.
And astronomers learn to grow and love these lines and identify them immediately in any spectrum, for they give you crucial information about the nature of the star, its age, its composition and so much more.
Have a great day!
*If you squint your eyes a bit more you can find other absorption lines from other atoms embedded in the spectrum as well.