By Diane Ackerman
The bestselling writer of A traditional background of the Senses now explores the attract of adultery, the charm of aphrodisiacs, and the cult of the kiss. Enchantingly written and stunningly proficient, this "audaciously wonderful romp during the global of romantic love" (Washington submit ebook global) is the following neatest thing to like itself.
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Extra resources for A Natural History of Love
Skeptics thus argued (and sometimes still do) that these systems might not after all be symbiotic. To overcome these arguments, two-micron spectroscopy has proved powerful. 5~ atmospheric window lie not only the steam bands, which depress the continua of M giants towards both ends of the window, but also the CO band heads. 3~ is a certain indicator of the presence of a cool star. By spectroscopy at these wavelengths, cool giants were shown to be present in the D-type objects He 2-38 and RR Tel (Alien et al 1978), and RX Pup (Barton, Phillips and Allen 1979).
I also have a question. Can you give an upper limit to the mass loss rate from ordinary symbiotic stars, which do not show radio emission? All normal red stars have winds, and it would be useful to have upper limits to the mass loss rate. Kwok: Not all normal red stars have winds. J. 165, 285) only red giants with spectral type later than M2-3 show wind characteristics. /v has to be> 10-8 (M@yr-1 )/(km s-1) assuming D~1 kpc. Kafatos: Is the shock arising from the colliding winds stationary, and what is the associated temperature?
3 cm flux density they measured in 1981 is lower than earlier measurements reported by Purton et al. (1981) and the turn-over frequency might have moved to 20 GHzin 1981 from 40 GHz a few years ago. In summary, there are probably two stellar winds in Vl016 Cygni (one from each stellar component) and their interaction may result in the shell structure seen by Newell and Hjellming (1981). The shell is probably moving at relatively low velocity, for after 16 years from the initiation of the new fast wind, the M-giant wind is still the dominant contributor to the radio emissions below 10 GHz.