# Molecules in stars

Stellar molecules are molecules that exist or form in stars. Such formations can take place when the temperature is low enough for molecules to form – typically around 6000 K or cooler.[1] Otherwise the stellar matter is restricted to atoms (chemical elements) in the forms of gas or – at very high temperatures – plasma.

## Background

Matter is made up by atoms (formed by protons and other subatomic particles). When the environment is right, atoms can join together and form molecules, which give rise to most materials studied in materials science. But certain environments, such as high temperatures, don't allow atoms to form molecules. Stars have very high temperatures, primarily in their interior, and therefore there are few molecules formed in stars. For this reason, a typical chemist (who studies atoms and molecules) would not have much to study in a star, so stars are better explained by astrophysicists or astrochemists. However, low abundance of molecules in stars is not equated with no molecules at all.[2]

## Evidence and research

Although the Sun is a star, its photosphere has a low enough temperature of 6,000 K (5,730 °C; 10,340 °F), and therefore molecules can form. Water has been found on the Sun, and there is evidence of H2 in white dwarf stellar atmospheres.[2][3]

Cooler stars include absorption band spectra that are characteristic of molecules. Similar absorption bands are found in sun spots which are cooler areas on the Sun. Molecules found in the Sun include MgH, CaH, FeH, CrH, NaH, OH, SiH, VO, and TiO. Others include CN CH, MgF, NH, C2, SrF, zirconium monoxide, YO, ScO, BH.[4]

Stars of most types can contain molecules, even the Ap category of A class stars. Only the hottest O, B and A class stars have no detectable molecules. Also carbon rich white dwarfs, even though very hot, have spectral lines of C2 and CH.[5]

### Laboratory measurements

Measurements of simple molecules that may be found in stars are performed in laboratories to determine the wavelengths of the spectra lines. Also, it is important to measure the dissociation energy and oscillator strengths (how strongly the molecule interacts with electromagnetic radiation). These measurements are inserted into formula that can calculate the spectrum under different conditions of pressure and temperature. However, man-made conditions are often different from those in stars, because it is hard to achieve the temperatures, and also local thermal equilibrium, as found in stars, is unlikely. Accuracy of oscillator strengths and actual measurement of dissociation energy is usually only approximate.[5]

### Model atmosphere

A numerical model of a star's atmosphere will calculate pressures and temperatures at different depths, and can predict the spectrum for different elemental concentrations.

## Application

The molecules in stars can be used to determine some characteristics of the star. The isotopic composition can be determined if the lines in the molecular spectrum are observed. The different masses of different isotopes cause vibration and rotation frequencies to significantly vary. Secondly the temperature can be determined, as the temperature will change the numbers of molecules in the different vibrational and rotational states. Some molecules are sensitive to the ratio of elements, and so indicate elemental composition of the star.[5] Different molecules are characteristic of different kinds of stars, and are used to classify them.[4] Because there can be numerous spectral lines of different strength, conditions at different depths in the star can be determined. These conditions include temperature and speed towards or away from the observer.[5]

The spectrum of molecules has advantages over atomic spectral lines, as atomic lines are often very strong, and therefore only come from high in the atmosphere. Also the profile of the atomic spectral line can be distorted due to isotopes or overlaying of other spectral lines.[5] The molecular spectrum is much more sensitive to temperature than atomic lines.[5]

## Detection

The following molecules have been detected in the atmospheres of stars:

Molecule Designation
AlH[6] Aluminium monohydride
AlO[6] Aluminium monoxide
C2[6] Diatomic carbon
CH[7] Carbyne
CN[7][8] Cyanide
CO[9] Carbon monoxide
CaCl[6] Calcium chloride
CaH[10] Calcium monohydride
CeH[11] Cerium monohydride
CeO[8] Cerium monoxide
CoH[6] Cobalt hydride
CrH[6] Chromium hydride
CuH[6] Copper hydride
FeH[11] Iron hydride
HCl[6] Hydrogen chloride
HF[6] Hydrogen fluoride
H2[3] Molecular hydrogen
LaO[6][8] Lanthanum oxide
MgH[12] Magnesium monohydride
MgO[8] Magnesium oxide
NH[7] Imidogen
NiH[6] Nickel hydride
OH[6] Hydroxide
ScO[6] Scandium oxide
SiH[6] Silicon monohydride
SiO[6] Silicon monoxide
TiO[13][14] Titanium oxide
YO[6][8] Yttrium oxide
ZnH[6] Zinc hydride
ZrO[6][8] Zirconium oxide
3 Atoms
HCN[6] Hydrogen cyanide
CO2[15] Carbon dioxide
SiC2[6] Silicon dicarbide
CaNC[16] Calcium isocyanide
CaOH[6] Calcium hydroxide
H2O[17] Water
4 Atoms
C2H2[6] Acetylene

## References

1. ^ Masseron, T. (December 2015), "Molecules in stellar atmospheres", in Martins, F.; Boissier, S.; Buat, V.; Cambrésy, L.; Petit, P. (eds.), SF2A-2015: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics, pp. 303–305, Bibcode:2015sf2a.conf..303M
2. ^ a b "Stellar Molecules » American Scientist". American Scientist. doi:10.1511/2013.105.403. Retrieved 24 October 2013. Cite journal requires `|journal=` (help)
3. ^ a b Xu, S.; et al. (2013). "Discovery of Molecular Hydrogen in White Dwarf Atmospheres". The Astrophysical Journal. 766 (2): L18. arXiv:1302.6619. Bibcode:2013ApJ...766L..18X. doi:10.1088/2041-8205/766/2/L18. ISSN 2041-8205.
4. ^ a b McKellar, Andrew (1951). "Molecules in Stellar Atmospheres". Astronomical Society of the Pacific Leaflets. 6 (265): 114. Bibcode:1951ASPL....6..114M.
5. Symposium, International Astronomical Union; Union, International Astronomical (1987). Astrochemistry. Springer Science & Business Media. p. 852. ISBN 9789027723604.
6. Tsuji, T. (1986). "Molecules in stars". Annual Review of Astronomy and Astrophysics. 24: 89–125. Bibcode:1986ARA&A..24...89T. doi:10.1146/annurev.aa.24.090186.000513.
7. ^ a b c Briley, Michael M.; Smith, Graeme H. (November 1993). "NH-, CH-, and CN-band strengths in M5 and M13 bright red giants". Astronomical Society of the Pacific. 105 (693): 1260–1268. Bibcode:1993PASP..105.1260B. doi:10.1086/133305.
8. Wyckoff, S.; Clegg, R. E. S. (July 1978). "Molecular spectra of pure S stars". Monthly Notices of the Royal Astronomical Society. 184: 127–143. Bibcode:1978MNRAS.184..127W. doi:10.1093/mnras/184.1.127.
9. ^ Ayres, T. R.; et al. (March 1981). "Far-Ultraviolet Fluorescence of Carbon Monoxide in the Red Giant Arcturus". Bulletin of the American Astronomical Society. 13: 515. Bibcode:1981BAAS...13..515A.
10. ^ Jao, W.-C. (December 2011). Johns-Krull, Christopher M.; Browning, Matthew K.; West, Andrew A. (eds.). There is Something About CaH. 16th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun. Proceedings of a conference held August 28- September 2, 2010 at the University of Washington, Seattle, Washington. ASP Conference Series. 448. San Francisco: Astronomical Society of the Pacific. p. 907. Bibcode:2011ASPC..448..907J.
11. ^ a b Clegg, R. E. S.; Lambert, D. L. (December 1978). "On the identification of FeH and CeO in S stars". Astrophysical Journal, Part 1. 226: 931–936. Bibcode:1978ApJ...226..931C. doi:10.1086/156674.
12. ^ Bonnell, J. T.; Bell, R. A. (September 1993). "Further Determinations of the Gravities of Cool Giant Stars Using MGI and MGH Features". Monthly Notices of the Royal Astronomical Society. 264 (2): 334. Bibcode:1993MNRAS.264..334B. doi:10.1093/mnras/264.2.334.
13. ^ Jorgensen, Uffe G. (April 1994). "Effects of TiO in stellar atmospheres". Astronomy and Astrophysics. 284 (1): 179–186. Bibcode:1994A&A...284..179J.
14. ^ Hauschildt, P.; et al. (2001). Woodward, Charles E.; Bicay, Michael D.; Shull, J. Michael (eds.). Cool Stellar Atmospheres. Tetons 4: Galactic Structure, Stars and the Interstellar Medium. ASP Conference Series. 231. San Francisco: Astronomical Society of the Pacific. p. 427. Bibcode:2001ASPC..231..427H. ISBN 1-58381-064-1.
15. ^ Cami, J.; et al. (August 2000). "CO2 emission in EP Aqr: Probing the extended atmosphere". Astronomy and Astrophysics. 360: 562–574. Bibcode:2000A&A...360..562C.
16. ^ Cernicharo, J.; et al. (July 2019). "Discovery of the first Ca-bearing molecule in space: CaNC". Astronomy & Astrophysics. 627: 5. arXiv:1906.09352. Bibcode:2019A&A...627L...4C. doi:10.1051/0004-6361/201936040. PMID 31327871. L4.
17. ^ Allard, F.; et al. (May 1994). "The influence of H2O line blanketing on the spectra of cool dwarf stars". The Astrophysical Journal. 426 (1): L39–L41. Bibcode:1994ApJ...426L..39A. doi:10.1086/187334.