Grade 9 Science Worksheets

Learning Objectives

• Define physical and chemical properties of matter.
• Identify examples of physical changes.
• Identify examples of chemical changes.+ Show more

Learning Objectives

• Identify examples of physical changes in matter.
• Distinguish between physical and chemical properties.
• Understand the difference between physical and chemical changes.

Learning Objectives

• Understand how external forces influence the motion of objects.
• Analyze free-body diagrams to identify net forces and predict acceleration.
• Apply Newton's second law to various scenarios involving forces and motion.+ Show more

Learning Objectives

• Understand the mathematical relationships governing gravitational and electrostatic forces.
• Apply inverse-square law formulas to calculate magnitudes of forces between objects.
• Determine the direction of forces using vector representation and Coulomb's and Newton's laws.+ Show more

Learning Objectives

• Describe the main stages of stellar evolution from star formation to terminal outcomes.
• Explain the role of Hertzsprung-Russell diagrams and spectral classification in understanding stars.
• Identify differences in stellar lifecycles based on mass and other properties.+ Show more

Learning Objectives

• Understand the components of water budgets and how surface and subsurface water flows are quantified.
• Relate precipitation, evapotranspiration, human withdrawals, and streamflow variability within hydrologic systems.
• Explain the impacts of altered hydrologic fluxes on geomorphic processes and sediment yield.+ Show more

Learning Objectives

• Understand the concept of scale in the solar system and how sizes and distances vary.
• Analyze planetary motion and how relative scale properties relate to observations.
• Connect apparent brightness and movement to actual distances and orbital periods.+ Show more

Learning Objectives

• Explain surface and subsurface water flow processes using water-budget frameworks.
• Interpret discharge hydrographs and groundwater level records for streamflow analysis.
• Relate precipitation, evapotranspiration, and human withdrawals to water resource variability.+ Show more

Learning Objectives

• Explain how paleoclimate proxies (ice cores, tree rings, marine sediments, and speleothems) provide evidence of past climate conditions.
• Interpret proxy indicators such as isotopic ratios, growth increments, and microfossil assemblages to reconstruct past variability.
• Describe how age models and uncertainty help connect proxy records to climate patterns over time.

Learning Objectives

• Understand the water-budget framework and how it quantifies surface and subsurface water flows.
• Interpret discharge hydrographs and groundwater level records to assess streamflow variability and aquifer sustainability.
• Relate precipitation inputs, evapotranspiration losses, and human withdrawals to changes in hydrologic fluxes.+ Show more

Learning Objectives

• Explain how scale affects perceived size and distance in the solar system
• Describe how brightness and apparent motion depend on distance and viewing perspective
• Use orbital period and relative distance to make qualitative predictions about planetary motion

Learning Objectives

• Identify the main components of the solar system
• Describe the relative sizes and distances of planets from the Sun
• Understand the concept of scale in astronomical observations+ Show more

Learning Objectives

• Explain how the protoplanetary disk contributed to planetary formation.
• Identify key evidence supporting planetary origins, such as meteorites and isotopic dating.
• Describe differences between inner rocky planets and outer gas giants based on formation processes.

Learning Objectives

• Explain how scale and distance affect how the solar system appears from Earth
• Use basic measurement ideas (relative scale, brightness, and apparent motion) to infer orbital properties
• Distinguish between physical distance/size and observational perspective when interpreting sky observations

Learning Objectives

• Explain how scale models help connect observable features of the night sky to real distances and sizes in the solar system.
• Describe how perspective affects apparent motion and brightness of planets as Earth orbits the Sun.
• Use relative reasoning about orbital periods and repeating patterns to interpret sky observations.

Learning Objectives

• Understand the processes involved in the carbon cycle
• Identify the roles of different organisms and environmental factors in carbon movement
• Explain how carbon cycles through air, water, soil, and living organisms

Learning Objectives

• Understand the spectrum of electromagnetic radiation and its relationship with photon energy.
• Explain how different types of electromagnetic waves interact with matter, including phenomena like atomic emission and absorption.
• Apply Planck’s relation to compare energies and wavelengths across the electromagnetic spectrum.+ Show more

Learning Objectives

• Understand the concept of gravitational and electrostatic forces.
• Learn the inverse-square law and its impact on force magnitude.
• Apply mathematical formulas to calculate forces between objects.+ Show more

Learning Objectives

• Explain how photon energy depends on frequency using Planck’s relation.
• Relate electromagnetic wave properties (frequency, wavelength) to how signals interact with matter.
• Interpret spectral features (emission and absorption lines) and connect them to atomic energy levels.+ Show more

Learning Objectives

• Explain Newton’s Third Law using the idea of action–reaction force pairs that act on different objects.
• Identify whether two forces form a Third Law pair by checking the interacting objects and direction.
• Use Third Law pairs to analyze everyday situations such as rockets, walking, and pushing against walls.

Learning Objectives

• Describe the processes involved in the formation of the solar system from a protoplanetary disk.
• Identify evidence such as meteorite composition and radiometric dating that support theories of planetary formation.
• Explain the differences between inner rocky planets and outer gas giants based on planetary differentiation and volatile content.+ Show more

Learning Objectives

• Explain how greenhouse gases trap heat in Earth's atmosphere.
• Describe the role of infrared radiation in Earth's energy balance.
• Analyze how variations in greenhouse gas concentrations affect global temperatures.

Learning Objectives

• Identify key components involved in molecular signaling pathways.
• Understand how signal transduction cascades influence gene expression.
• Explain mechanisms of hormonal and receptor-ligand signaling.+ Show more

Learning Objectives

• Explain how net external force relates to acceleration using Newton’s second law
• Use free-body diagrams to identify and sum all forces acting on an object
• Predict changes in motion for scenarios involving contact forces and field forces (including tension and friction)

Learning Objectives

• Understand the wave and photon descriptions of electromagnetic radiation.
• Relate frequency and wavelength to photon energy and interaction with matter.
• Explain phenomena such as atomic emission and absorption lines, signal transmission, and spectral attenuation.+ Show more

Learning Objectives

• Identify observable signs of chemical reactions, such as gas formation, precipitate production, color change, temperature change, and odor change.
• Understand how these signs relate to changes in atomic arrangements and bonding patterns.
• Recognize examples of oxidation and combustion reactions based on observable evidence.

Learning Objectives

• Explain how greenhouse gases affect Earth’s energy flow by absorbing and re-emitting infrared radiation.
• Describe how energy balance depends on absorption, re-emission, and the altitude where radiation escapes to space.
• Use greenhouse-effect concepts to predict how changes in greenhouse gas concentrations can change surface temperature.

Learning Objectives

• Understand the formation of the solar system from a rotating protoplanetary disk.
• Identify key evidence supporting planetary formation theories, such as meteorite composition and radiometric dating.
• Explain the differences between inner rocky planets and outer gas giants based on planetary differentiation and volatile content.+ Show more

Learning Objectives

• Understand the basic concepts of force and motion.
• Identify different types of forces such as contact and field forces.
• Interpret free-body diagrams and apply Newton's second law.+ Show more

Learning Objectives

• Understand the formation process of the solar system from a protoplanetary disk.
• Identify evidence supporting planetary formation theories, including meteorite composition and isotopic radiometric dating.
• Explain differences between inner rocky planets and outer gas giants based on planetary differentiation and volatile content.+ Show more

Learning Objectives

• Describe the formation processes of the solar system from a protoplanetary disk.
• Identify evidence supporting planetary formation theories, including meteorite composition and isotopic dating.
• Explain the differences between inner rocky planets and outer gas giants based on planetary differentiation and volatile content.+ Show more

Learning Objectives

• Understand the inverse-square dependence of gravitational and electrostatic forces.
• Apply quantitative formulas to calculate magnitudes and directions of forces between masses and charges.
• Explain the approximations used for point masses and point charges in force calculations.+ Show more

Learning Objectives

• Understand and quantify surface and subsurface water flows using water-budget frameworks
• Relate precipitation, evapotranspiration, and human withdrawals to streamflow and aquifer health
• Analyze the impact of altered hydrologic fluxes on geomorphic processes+ Show more

Learning Objectives

• Understand the main stages of stellar evolution and their characteristics.
• Identify different end states of stars such as white dwarfs, neutron stars, and black holes.
• Describe how nucleosynthesis contributes to elemental formation in stars.+ Show more

Learning Objectives

• Understand the processes involved in planetary formation from a protoplanetary disk.
• Identify key evidence supporting models of planetary origins, such as meteorite composition and isotopic dating.
• Explain the differences in composition and structure between inner rocky planets and outer gas giants.+ Show more

Learning Objectives

• Understand the formation of the solar system from a protoplanetary disk.
• Identify evidence supporting planetary formation theories.
• Describe the differences between inner rocky planets and outer gas giants.+ Show more

Learning Objectives

• Understand the stages of star formation and evolution
• Identify key features of stellar life cycles from gas clouds to final remnants
• Interpret Hertzsprung-Russell diagrams and spectral classifications+ Show more

Learning Objectives

• Explain how angular momentum in a rotating protoplanetary disk can lead to planet formation.
• Describe how meteorite composition and isotopic radiometric dating provide evidence for solar system chronology.
• Connect volatile gradients and planetary differentiation to the rocky inner planets and gas-rich outer planets.

Learning Objectives

• Describe the formation process of the solar system from a protoplanetary disk.
• Identify key evidence supporting planetary formation theories such as meteorite composition and radiometric dating.
• Explain differences between inner rocky planets and outer gas giants based on gradients in volatile content.+ Show more

Learning Objectives

• Identify parts of the electromagnetic spectrum and understand their relative frequencies.
• Explain how photon energy relates to wave frequency.
• Understand phenomena such as atomic emission and absorption lines.+ Show more

Learning Objectives

• Explain how stellar mass affects the path of stellar evolution from formation through later stages.
• Describe how nuclear fusion processes change during a star’s main-sequence and post-main-sequence evolution.
• Interpret how Hertzsprung–Russell (H–R) diagrams, spectral classification, and supernova remnants provide evidence for evolution.

Learning Objectives

• Describe the processes involved in stellar formation and evolution.
• Identify the stages of stellar evolution from main sequence to terminal outcomes.
• Explain the use of Hertzsprung-Russell diagrams and spectral classification in understanding stars.+ Show more

Learning Objectives

• Understand the different types of force interactions in physics.
• Identify examples of forces and their effects.
• Explain Newton's third law of motion.+ Show more

Learning Objectives

• Understand the process of star formation from clouds of gas and dust.
• Identify characteristics of stars on the main sequence.
• Describe different stages of stellar evolution including red giant phase, white dwarf, neutron star, and black hole outcomes.+ Show more

Learning Objectives

• Understand the mathematical forms of gravitational and electrostatic force equations.
• Predict magnitudes and directions of forces between masses and charged objects using inverse-square laws.
• Apply vector concepts to analyze net forces in various scenarios.+ Show more

Learning Objectives

• Describe the main stages of stellar evolution from star formation to terminal outcomes.
• Interpret Hertzsprung-Russell diagrams and spectral classifications of stars.
• Explain the processes of nucleosynthesis and element enrichment in the interstellar medium.+ Show more

Learning Objectives

• Explain the stages of stellar evolution from star formation to end states.
• Interpret Hertzsprung-Russell diagrams and relate spectral classifications to star characteristics.
• Describe processes such as supernovae, nucleosynthesis, and elemental enrichment of the interstellar medium.

Learning Objectives

• Describe how stars form and evolve through the main sequence and later stages based on mass
• Explain how Hertzsprung-Russell diagrams and spectral classification provide evidence for stellar properties
• Compare terminal outcomes of stellar evolution (white dwarfs, neutron stars, black holes) and connect them to nucleosynthesis