Joint ING and NOT Conference: Second Meeting on Hot Subdwarf Stars and Related Objects
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ING Newsletter No. 9, March 2005

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Reference: ING Newsl., No. 9, page 32.
Article mirrored at: La Palma server | Cambridge server
Other available formats: PDF

Joint ING and NOT Conference: Second Meeting on Hot Subdwarf Stars and Related Objects 

Together with the Nordic Optical Telescope, the ING is organising a meeting with the title “Hot Subdwarf Stars and Related Objects”, to be held on La Palma from the 6 to 10 of June this summer. The conference venue is the Real Club Náutico of Santa Cruz de La Palma, and it will be the first major astronomy conference to be held  in the home town of the ING’s sea-level offices.

Figure 1

Financial support has been given by the organisers, the Excmo. Cabildo Insular de La Palma (local government) and the Patronato de Turismo de La Palma (tourist board). Additionally the Real Club Náutico has been extremely helpful by making their facilities available to us at no cost.

This conference is the second meeting on hot subdwarf stars, a new biennial series that was started at Keele University in 2003. It is an offspring of the long running White Dwarf meetings, which counted their 14th meeting last year. The intention is that the Subdwarf meetings will also run every second year, in the odd years between the WD meetings. The aim of the workshop series is to disseminate recent results on the properties, formation, and evolution of the hot subdwarf stars and related objects, and to assess the impact of these results on other areas of astrophysics.

Hot subdwarf stars are extreme horizontal branch (EHB) stars and pre-white dwarf stars. The EHB stars are core helium-burning stars with extremely thin hydrogen envelopes, and form the majority of bright stars in surveys for extremely blue objects, where they are classified as subdwarf-B (sdB) stars. They also appear in the colour-magnitude diagrams of some globular clusters as an extension of the blue tail formed by classical horizontal branch stars, though it is not clear why some clusters show this feature and others do not. The pre-white dwarf stars are related to the sdBs, but have exhausted their capacity to burn helium in the core. Many of the brightest hot subdwarfs in the field are of this class, and they are classified as sdO stars.

Topics for the meeting includes: Evolutionary models and the UV-upturn phenomenon; hot subdwarfs and hot HB stars in the field, clusters and galaxies; hot subdwarfs in binary systems; atmospheric properties of hot subdwarf stars; asteroseismology of sdB stars, and progenitors and progeny of sdB stars.

The capacity of the conferences is limited by the size of the available facilities to about 90 people. More information can be found on the ING web-pages, at The registration is open until April 1. ¤

*: Email contact: Roy H. Østensen on behalf of the Local Organising Committe (

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