Originally released via Stevenson, Inc., this sensible source profiles over 100 winning and ecocnomic occasions for nonprofit organizations.
Examples of occasions profiled include:
- Donor luncheons
- Community health center days
- Award ceremonies
- Fundraising auctions
- Holiday events
- Student dances
- Cocktail parties
- Home tours
- Athletic events
- Boutiques partnerships
- Extreme fundraising events
- Gambling events
- College nights
- Women’s nights
- Singles events
- Family-oriented events
- Fashion shows
- Antique shows
- Black-tie events
Please observe that a few content material featured within the unique model of this identify has been got rid of during this released model because of permissions issues.Content:
Chapter 1 video game, Contest and Team?Oriented Fundraisers (pages 4–8):
Chapter 2 occasions Geared to girls (pages 9–13):
Chapter three Galas and High?End occasions (pages 14–19):
Chapter four outside occasions (pages 20–27):
Chapter five nutrients? and Refreshment?Centered occasions (pages 28–33):
Chapter 6 fairs and Community?Friendly occasions (pages 34–41):
Chapter 7 occasions that contain College?aged, institution members (pages 42–44):
Chapter eight Themed and interval occasions (pages 45–51):
Chapter nine Auctions and Raffles (pages 52–57):
Chapter 10 vacation orientated occasions and Fundraising tasks (pages 58–60):
Chapter eleven occasions with a distinct Twist (pages 61–66):
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Extra info for Best Ever Directory of Special Events, Fifth Edition
This dead layer crucially modi®es the spectral response of the detector from a few to a few tens of kiloelectronvolts, its impact on the analysis of GRB spectra below 60 keV has been studied by Niel, Jourdain, and Roques (1990). This problem can be avoided by using cleaved crystals as in HETE-Fregate (see Chapter 4). Finally, doubts on the presence of lines can also arise from the large number of GRB spectra which are treated and for a given burst the number of spectra which are analyzed with dierent timescales.
Finally, as we have said, the reverse shock is not taken into account. Even though this basic model was successful in explaining the ®rst BeppoSAX results, it quickly became necessary to consider more complex conditions. These conditions are presented in the second part of Chapter 6. The following elements have been progressively added to complete the basic ®reball model: xxxiv . . . Introduction Introduction of the reverse shock (within the ejecta), which can explain the strong optical ¯ashes and radio ¯ares.
But is is clear that the Konus instruments have provided the most important and homogeneous population of GRBs presenting features around 400 keV in emission and 30±70 keV in absorption. 14 The early times [Ch. 1 Nevertheless the reality of these features raised a lot of debates. A line seen by one group was not always con®rmed by another observing the same burst with a dierent instrument. For GRB 811231, for example, the gamma-ray spectrometer of SMM exhibited no evidence for the presence of an emission feature reported by Konus between 400 and 500 keV (Nolan et al.
Best Ever Directory of Special Events, Fifth Edition