Lab report, bean bag and water bottle lab Directions
Now that the lab is complete, it is time to write your lab report. The purpose of this guide is to help you write a clear and concise report that summarizes the lab you have just completed.
The lab report is composed of four sections:
Section I: Experimental Overview
Provide background information.
Include the hypothesis(es).
Summarize the procedures.

Section II: Data and Observations
Summarize the data you collected in the lab guide.
Include information from data tables.
Include any written observations that are relevant.

Section III: Analysis and Discussion
Discuss any important calculations or formulas used.
Identify key results, what the results indicate, and any trends in the data.
Include graphs (if constructed) that display trends in the data.
Provide possible reasons for any problems with the experiment, or unexpected data.

Section IV: Conclusions
Identify if the hypothesis(es) was (were) supported or refuted.
Provide logical reasoning based on data.
Explain how the experiment could be improved.

To help you write your lab report, you will first answer the questions listed below by reflecting on the experiment you have just completed. Then you will use the answers to these questions to write the lab report that you will turn into your teacher.
You can upload your completed report with the upload tool in formats such as OpenOffice. org, Microsoft Word, or PDF. Alternatively, your teacher may ask you to turn in a paper copy of your report or use a web-based writing tool.
Questions

Section I: Experimental Overview

What is the purpose of the lab, the importance of the topic, and the question you are trying to answer?

What is your hypothesis (or hypotheses) for this experiment?

What methods are you using to test this (or each) hypothesis?

Section II: Data and Observations
Locate the data and observations collected in your lab guide. What are the key results? How would you best summarize the data to relate your findings?

Do you have quantitative data (numerical results or calculations)? Do you have qualitative data (written observations and descriptions)? How can you organize this date for your report?

Section III: Analysis and Discussion

What do the key results indicate?

If you constructed graphs, what trends do they indicate in your data?

Were there any problems with the experiment or the methods? Did you have any surprising results?

Section IV: Conclusions

What do the results tell you about your hypothesis(es)?

How do the data support your claim above?

If you could repeat the experiment and make it better, what would you do differently and why?

  sequence  is a continuous and distinctive band of  stars  that appears on plots of stellar  color  versus  brightness. these color-magnitude plots are known as  hertzsprung–russell diagramsafter their co-developers,  ejnar hertzsprungand  henry norris russell. stars on this band are known as  main-sequence stars  or  dwarf stars. these are the most numerous true stars in the universe, and include the earth's  sun.after condensation and ignition of a star, it generates  thermal energy  in its dense core region through  nuclear fusion  of  hydrogen  into  helium. during this stage of the star's lifetime, it is located on the main sequence at a position determined primarily by its mass, but also based upon its chemical composition and age. the cores of main-sequence stars are in  hydrostatic equilibrium, where outward thermal pressure from the hot core is balanced by the inward pressure of  gravitational collapse  from the overlying layers. the strong dependence of the rate of energy generation on temperature and pressure to sustain this balance. energy generated at the core makes its way to the surface and is radiated away at the  photosphere. the energy is carried by either  radiation  or  convection, with the latter occurring in regions with steeper temperature gradients, higher opacity or both.the main sequence is sometimes divided into upper and lower parts, based on the dominant process that a star uses to generate energy. stars below about 1.5 times the  mass of the sun  (1.5  m☉) primarily fuse hydrogen atoms together in a series of stages to form helium, a sequence called the  proton–proton chain. above this mass, in the upper main sequence, the nuclear fusion process mainly uses atoms of  carbon,  nitrogen  and  oxygen  as intermediaries in the  cno cycle  that produces helium from hydrogen atoms. main-sequence stars with more than two solar masses undergo convection in their core regions, which acts to stir up the newly created helium and maintain the proportion of fuel needed for fusion to occur. below this mass, stars have cores that are entirely radiative with convective zones near the surface. with decreasing stellar mass, the proportion of the star forming a convective envelope steadily increases. main-sequence stars below 0.4  m☉undergo convection throughout their mass. when core convection does not occur, a helium-rich core develops surrounded by an outer layer of hydrogen.in general, the more massive a star is, the shorter its lifespan on the main sequence. after the hydrogen fuel at the core has been consumed, the star  evolves  away from the main sequence on the hr diagram, into a  supergiant,  red giant, or directly to a  white dwarf.